SlideShare ist ein Scribd-Unternehmen logo
1 von 21
Downloaden Sie, um offline zu lesen
D RAFT VERSION A PRIL 12, 2011
                                               Preprint typeset using LTEX style emulateapj v. 11/10/09
                                                                      A




                                                     INVESTIGATING THE NUCLEAR ACTIVITY OF BARRED SPIRAL GALAXIES: THE CASE OF NGC 1672
                                             L. P. J ENKINS 1,2 , W. N. B RANDT 3,4 , E. J. M. C OLBERT 2 , B. KORIBALSKI 5 , K. D. K UNTZ 2 , A. J. L EVAN 6 , R. O JHA 7 , T. P. ROBERTS 8 ,
                                                                                                      M. J. WARD 8 , A. Z EZAS 9
                                                                                                              Draft version April 12, 2011

                                                                                                         ABSTRACT
                                                           We have performed an X-ray study of the nearby barred spiral galaxy NGC 1672, primarily to ascertain the
arXiv:1104.1649v1 [astro-ph.CO] 8 Apr 2011




                                                        effect of the bar on its nuclear activity. We use both Chandra and XMM-Newton observations to investigate
                                                        its X-ray properties, together with supporting high-resolution optical imaging data from the Hubble Space
                                                        Telescope (HST), infrared imaging from the Spitzer Space Telescope, and ATCA ground-based radio data.
                                                        We detect 28 X-ray sources within the D25 area of the galaxy, many of which correlate spatially with star-
                                                        formation in the bar and spiral arms, while two are identified as background galaxies in the HST images. Nine
                                                        of the X-ray sources are ULXs, with the three brightest (LX > 5 × 1039 erg s−1 ) located at the ends of the
                                                        bar. With the spatial resolution of Chandra, we are able to show for the first time that NGC 1672 possesses
                                                        a hard (Γ ∼ 1.5) nuclear X-ray source with a 2–10 keV luminosity of 4 × 1038 erg s−1 . This is surrounded
                                                        by an X-ray bright circumnuclear star-forming ring, comprised of point sources and hot gas, which dominates
                                                        the 2–10 keV emission in the central region of the galaxy. The spatially resolved multiwavelength photometry
                                                        indicates that the nuclear source is a low-luminosity AGN (LLAGN), but with star formation activity close to
                                                        the central black hole. A high-resolution multiwavelength survey is required to fully assess the impact of both
                                                        large-scale bars and smaller-scale phenomena such as nuclear bars, rings and nuclear spirals on the fueling of
                                                        LLAGN.
                                                        Subject headings: galaxies: individual (NGC 1672) – galaxies: nuclei – galaxies: spiral – galaxies: evolution

                                                                          1. INTRODUCTION                                      material is also believed to build ‘pseudobulges’, which are
                                                The presence of a bar in a galaxy plays an impor-                              distinct from classical galaxy bulges (Kormendy & Kennicutt
                                             tant role in its evolution. Approximately two-thirds of                           2004). A strong global density pattern such as a bar can also
                                             all spiral galaxies are barred (e.g. Eskridge et al. 2000;                        produce a series of resonances between the angular velocity
                                             Men´ ndez-Delmestre et al. 2007), so any complete picture of
                                                  e                                                                            of the bar and the orbital motions of stars and gas in the disk,
                                             galaxies must include the impact of bars on both their nu-                        where rings can form (Buta 1999). Indeed, some galaxies
                                             clear and extra-nuclear properties. Secular (i.e. internal)                       with bars are known to have circumnuclear rings of star for-
                                             galaxy evolution involving bars, oval distortions and spiral                      mation (e.g. Buta & Combes 1996; Knapen 2005a), resulting
                                             structure can have a significant effect when a galaxy is no                        from increased gas density at or near the Inner Lindblad Res-
                                             longer merging or interacting strongly with other galaxies (see                   onance (ILR).
                                             Kormendy & Kennicutt 2004). For example, there is believed                           A question that we are addressing with this study is, can the
                                             to be a causal connection between the existence of a bar and                      material driven to the center of a galaxy by the bar also fuel
                                             a galaxy’s circumnuclear properties. Bars can drive gas from                      an active galactic nucleus (AGN)? While there is clear obser-
                                             the outer disk to the inner regions of the galaxy; gas clouds                     vational evidence that bars in disk galaxies cause higher cen-
                                             are shocked as they encounter the leading edge of the bar,                        tral concentrations of gas (and hence centrally concentrated
                                             lose angular momentum, and flow towards the galaxy’s center                        star formation) compared to non-barred galaxies, it is unclear
                                             (Shlosman et al. 1990). An observable result of this is that a                    whether a large-scale bar is sufficient to transport material
                                             substantial fraction of galaxies with bars show enhanced star-                    close enough for AGN feeding (typically on AU scales, see
                                             formation activity in their central regions, and the inflow of                     Knapen 2005b for a review). Additionally, in an X-ray study
                                                                                                                               by Maiolino et al. (1999) using Ginga, ASCA and BeppoSAX
                                                                                                                               data, a strong correlation was found between absorbing col-
                                                  1 Laboratory for X-ray Astrophysics, NASA Goddard Space Flight Cen-
                                                                                                                               umn density toward Type-2 Seyfert nuclei and the presence
                                               ter, Code 662, Greenbelt, MD 20771, USA                                         of a strong bar, i.e. more than 80% of Compton-thick Seyfert
                                                  2 Johns Hopkins University, 3400 N. Charles St, Baltimore, MD 21218,
                                               USA                                                                             2s are barred. This suggests that if a low-luminosity AGN
                                                  3 Department of Astronomy & Astrophysics, The Pennsylvania State             (LLAGN) is present, it may be obscured from view at optical
                                               University, 525 Davey Lab, University Park, PA 16802, USA                       wavelengths and/or diluted by strong star-formation activity,
                                                  4 Institute for Gravitation and the Cosmos, The Pennsylvania State Uni-
                                                                                                                               which could lead to a misclassification as a pure star-forming
                                               versity, University Park, PA 16802, USA
                                                  5 CSIRO, Australia Telescope National Facility (ATNF), PO Box 76,            nucleus.
                                               Epping NSW 1710, AUSTRALIA                                                         The topic of the influence of bars on galaxy evolution is
                                                  6 Department of Physics, University of Warwick, Coventry, CV4 7AL,           not well studied at X-ray energies, but we are now able
                                               UK                                                                              to utilize the excellent complementary imaging and spec-
                                                  7 NVI/United States Naval Observatory, 3450 Massachusetts Ave NW,
                                                                                                                               tral capabilities of Chandra and XMM-Newton to make de-
                                               Washington DC 20392, USA
                                                  8 Department of Physics, Durham University, South Road, Durham,              tailed investigations of the X-ray characteristics of these sys-
                                               DH1 3LE, UK                                                                     tems. In particular, high-spatial-resolution X-ray observa-
                                                  9 Department of Physics, University of Crete, PO Box 2208, GR-71003          tions with Chandra provide an ideal method for search-
                                               Heraklion, Greece                                                               ing for low-level AGN activity in nearby galaxies, in the
2                                                            Jenkins et al.

form of a hard central point source that may not be vis-              ring of star formation, measuring ∼ 11′′ × 9′′ (0.9 × 0.7 kpc
ible at other wavelengths. It also allows us to separate              at a distance of 16.3 Mpc), located between two ILRs. There-
potential AGN activity from other types of X-ray sources              fore, studies of its nuclear properties that use large apertures
that may reside close to the nucleus, such as X-ray bina-             are strongly affected by the star-formation in the ring. For
ries (XRBs) associated with circumnuclear star-formation.             example, Osmer et al. (1974) showed that the optical emis-
Indeed, X-ray surveys utilizing Chandra have proved suc-              sion spectrum in the central 17′′ was similar to those of
cessful in recent years in identifying previously unknown             normal HII nuclei, but with an Hα/Hβ ratio indicative of
LLAGN activity in nearby galaxies. In particular, X-ray nu-           a large amount of dust reddening. Storchi-Bergmann et al.
clei spanning a wide range of X-ray luminosities (∼ 1037 −            (1995) also measured optical emission-line ratios in a rela-
1044 erg s−1 , 2–10 keV) have been detected in a large frac-          tively large 10′′ × 20′′ aperture, and classified the nucleus as
tion (typically ∼45–70%) of galaxies hosting low-ionization           ‘composite’, with ratios between those of typical starburst and
nuclear emission regions (LINERs; Heckman 1980), as well              Seyfert values. More recent optical line ratio diagnostics by
as galaxies classed as having HII or transition nuclei (e.g.          Kewley et al. (2000) of the emission within a ∼ 13′′ slit are
Ho et al. 2001; Terashima & Wilson 2003; Satyapal et al.              indicative of an HII-type nucleus, with no Hα line broadening
2004; Satyapal et al. 2005; Dudik et al. 2005; Flohic et al.          detected. All of these studies will have been strongly contam-
2006; Gonz´ lez-Mart´n et al. 2006; Gonz´ lez-Mart´n et al.
              a         ı                      a         ı            inated by the emission from the circumnuclear starburst ring;
2009; Zhang et al. 2009; Desroches & Ho 2009). Studies at             however they do demonstrate that this component is domi-
other wavelengths have also recently been used to uncover             nant, and that any potential AGN activity would be relatively
previously unknown AGN activity in nearby galaxies. For               weak.
example, Spitzer infrared (IR) spectroscopic surveys have re-            More detailed, spatially resolved studies have also given
vealed bonafide AGN in both LINERs and IR-bright galax-                ambiguous results. Veron et al. (1981) detected possible
ies, some of which showed no sign of such activity in opti-           broadening of [O III] (∼300 km s−1 ) compared to Hβ lines
cal studies (Dudik et al. 2009; Goulding & Alexander 2009).           (∼150 km s−1 ) in the central 2′′ × 4′′ , which they sug-
High-resolution radio imaging has been shown to be an effi-            gested was evidence of a composite HII/Seyfert 2 nu-
cient method for finding LLAGN activity; compact radio nu-             cleus. Garcia-Vargas et al. (1990) performed a high-spatial-
clei have been found in 50% of LINERs/LLAGN, which are                resolution spectral analysis of the nucleus, and found a strong
thought to be attributable to relativistic jets produced by ac-       increase in the [O III]/Hβ ratio in the central 1′′ compared
creting super-massive black holes (Nagar et al. 2005 and ref-         to its immediate surroundings. However, both lines had the
erences therein).                                                     same FWHM of ∼300 km s−1 , and the authors classified
   To begin to address the nature of the nuclear (and off-            the nucleus as a LINER. Storchi-Bergmann et al. (1996) also
nuclear) X-ray emission in barred galaxies, we have con-              measured spatially-resolved (2′′ ) emission-line ratios, which
ducted a pilot study of the barred galaxy NGC 1672, using             were better modeled by a LINER-type stellar photoionization
X-ray observations from both Chandra (40 ks) and XMM-                 model with Tef f ≥ 45, 000 K, rather than photoionization by
Newton (50 ks). Here we report the results from these ob-             a strong AGN continuum.
servations, and use supporting HST/ACS, Spitzer and ATCA                 NGC 1672 has previously been observed with at X-ray
radio observations to assist in the interpretation of the X-ray       wavelengths with ROSAT and ASCA. Three bright X-ray
results. This paper is laid out as follows. In § 2 we give back-      sources were detected in the soft 0.2–2.0 keV band with the
ground information on the target galaxy NGC 1672. In § 3, we          ROSAT HRI and PSPC, which were clearly associated with
describe the Chandra, XMM-Newton, HST/ACS, Spitzer and                the galaxy (Brandt et al. 1996; de Naray et al. 2000). The
ATCA radio observations and data analysis techniques, and             brightest source was located at the nucleus, and the other two
in § 4 we present our results. In § 5 we discuss the nature of        were cospatial with the ends of the bar. The nucleus had a
the nuclear emission, and in § 6 we compare our results with          soft X-ray spectrum consistent with thermal emission with
those for other barred and non-barred galaxies in the litera-         a temperature of 0.68 keV, with a soft X-ray luminosity of
ture. Throughout this paper we use a distance to NGC 1672             7 × 1039 erg s−1 (0.2–2.0 keV). However, these studies were
of 16.3 Mpc, corresponding to a recession velocity of 1140 km         again unable to resolve the nuclear emission spatially due to
s−1 relative to the centroid of the Local Group (Osmer et al.         the 5′′ FWHM of the HRI point-spread-function (PSF), and
1974), with H0 =70 km s−1 Mpc−1 .                                     so could not determine whether the bulk of the soft emission
                                                                      came from a starburst or AGN. Furthermore, the ASCA data
                         2. NGC 1672
                                                                      showed no evidence of significant hard (2–10 keV) emission
   For this pilot study, we have selected the nearby (16.3 Mpc)       from the nuclear source, with the hard emission in the galaxy
late-type barred spiral galaxy NGC 1672 (SB(r)bc). It                 being dominated by two off-nuclear X-ray sources (X-3 and
has a moderately low inclination angle (i = 34◦ ,                     X-7, see figure 4b in de Naray et al. 2000). Thus, it was con-
de Vaucouleurs et al. 1991), and is known to have a strong            cluded that if an active nucleus is present in NGC 1672, it
bar (2.4′ in length, corresponding to 11.4 kpc at a distance          must be Compton-thick, with NH > 2 × 1024 cm−2 .
of 16.3 Mpc), many HII regions in its four spiral arms, plus
vigorous star formation at the ends of the bar (Brandt et al.
1996, and references therein). It has a high IR luminosity (log                  3. OBSERVATIONS AND DATA REDUCTION
LF IR /L⊙ = 10.2), and a global star formation rate (SFR) of
2.7 M⊙ yr−1 (Kewley et al. 2000).                                                      3.1. Chandra Observations
   Optical studies have given conflicting evidence as to the             NGC 1672 was observed with Chandra for 40 ks on April
nature of the nuclear activity in NGC 1672. It was noted              30, 2006 (ObsID 5932) using the back-illuminated S3 chip
by S´ rsic & Pastoriza (1965) as having a complex or ‘amor-
     e                                                                of the Advanced CCD Imaging Spectrometer (ACIS). The
phous’ nuclear morphology, and was subsequently shown by              field of view of the observation is shown in Figure 1; the
Storchi-Bergmann et al. (1996) to possess a circumnuclear             nucleus of the galaxy was placed at the aimpoint of the S3
Investigating the nuclear activity of barred spiral galaxies                                            3




                                    1’


Figure 1.DSS optical image of NGC1672 showing the Chandra ACIS-S field of view (solid red), the HST/ACS field of view
(dotted blue), and the 3- and 6-cm radio beam sizes (dashed green circles of 5.5′ and 9.8′ diameters respectively). The D25
ellipse of the galaxy is shown with a solid (black) line. The XMM-Newton and Spitzer observations cover the D25 area of the
galaxy. North is up, east to the left.

chip, and the observation encompasses the entire D25 10 ex-                      Initial detection of candidate sources was carried out in
tent of the galaxy. The data were initially processed with the                each energy-band image using the CIAO task wavdetect,
Chandra Interactive Analysis of Observations (CIAO) tool                      a Mexican Hat wavelet source detection algorithm. Wavelet
suite version 3.3, with CALDB version 3.2.1. The process-                     scales of 1.0, 1.414, 2.0, 2.828, 4.0, 5.657 & 8.0 pixels were
ing included a charge transfer efficiency (CTI) correction and                 used, and the significance threshold was set to 1.0 × 10−6
time-dependent gain correction. Further data analysis was                     corresponding to approximately one false detection per band
performed using CIAO version 3.4. A full-field light curve                     over the 8×8′ field. A merged source list was created that in-
was extracted from the level-2 event list to search for periods               cluded sources detected in all bands, which was used as the in-
of high background, but no strong flares were found, leaving                   put list for source parameterization in the ACIS Extract12
a net exposure time of 39.6 ks.                                               IDL software (AE; Broos et al. 2010). The main steps in the
                                                                              procedure are (1) the definition of source extraction regions
                 3.1.1. Imaging & Source Detection                            based on the 90% contour of the local PSF, (2) trial extrac-
                                                                              tion of events within those regions, (3) improvement of po-
  The basic data reduction was done using standard CIAO                       sitions if necessary (see below), (4) full extraction of source
data analysis threads.11 Images were created of an 8′ ×8′                     and background spectra using final positions, and the creation
region (encompassing the full D25 area of the galaxy) at                      of associated RMFs and ARFs for each source.
full 0.492′′ pixel resolution in soft (0.3–1 keV), medium                        Source positions were improved (in step 3) using the
(1–2 keV), hard (2–10 keV) and broad (0.3–10 keV) energy                      CHECK POSITIONS stage, which computes “mean data”
bands. Monochromatic exposure maps were created at 0.8,                       and “correlation” positions for all sources. The “mean data”
1.0 and 2.0 keV, corresponding to the peak energy in the soft,                position corresponds to the central position of the extracted in-
medium and hard band data. The images were adaptively                         band events in the 0.3–10 keV band, while the “correlation”
smoothed using the csmooth task, with a fairly low sig-                       positions are obtained by convolving the data image with a
nificance of 2σ above the local background (corresponding                      position-dependent model PSF. The offsets between these and
to ∼1–30 pixels in the body of the galaxy) to avoid over-                     the original wavdetect positions were typically 0.1–0.8′′.
smoothing of faint features in the central region (see § 4.3).                The position estimates were visually reviewed, and the best
   10 D
                                                                              was chosen for each source. Where there was little difference
         25 = the apparent major isophotal diameter measured at the surface
brightness level µB = 25.0 mag/arcsec2
   11 http://asc.harvard.edu/ciao/threads/index.html                            12   http://www.astro.psu.edu/xray/docs/TARA/ae users guide.html
4                                                             Jenkins et al.

between the estimates, the original position was retained.             data (images and spectra) were created using standard pat-
   The source extraction regions were based on the 90% con-            terns corresponding to single and double pixel events for the
tour of the local PSF at the final positions. Background spec-          PN (0–4), and patterns 0–12 (single to quadruple events) for
tra were extracted in local annuli, with inner radii of 1.1 times      the MOS cameras. For spectral extraction, the quality flag
of the 99% radius of the PSF (to exclude any residual source           was set to zero to reject events from bad pixels and events too
flux), and outer radii tailored so that each background spec-           close to the CCD chip edges.
trum contains at least 100 counts. For the central (ring) re-
gion, the whole area (17′′ radius) was masked out from the                                3.2.1. Imaging & Source Detection
background map due to the clumpy diffuse emission in the                 Multi-band source detection was performed on the PN and
area, and the background subtraction for sources in this re-           MOS data, using the methods detailed in Jenkins et al. (2005).
gion (except for the nucleus) was performed using the area             In brief, images were created in the following energy bands:
immediately outside this.                                              soft (0.3–1 keV), medium (1–2 keV) and hard (2–10 keV). Ex-
   Due to the complexity of the central region, the spec-              posure maps were created for each instrument/energy band
trum of the nuclear X-ray source was extracted manually in             using the SAS task EEXPMAP, and detector masks were cre-
CIAO using specextract. The source aperture was set                    ated for each camera with EMASK. Two methods of initial
to 1.2′′ radius, centered on the position from wavdetect               source recognition were used: EBOXDETECT, a sliding-box
(04h45m 42.5s , −59◦ 14′ 50.1′′ ). The local background flux            algorithm that simultaneously searches the three energy band
was measured in an annulus immediately outside this (1.2–              images, and EWAVELET, a Mexican hat wavelet detection
2.0′′ radius), and was chosen using the radio contours as a            routine that works on individual images. Both used back-
guide in order to cover as much of the area inside the ring,           ground maps created with ASMOOTH. The source lists from
without encountering any ring emission (see § 4.3). Any other          both methods were then parameterized using EMLDETECT,
typical non-local background region would have left residual           which performs maximum likelihood PSF fits to each source.
soft emission in the nuclear source counts.                            These were then compared, and any additional sources de-
   Since there is significant diffuse emission in the circum-           tected with EWAVELET were added to the EBOXDETECT
nuclear ring area, it is possible that some of the candidate           source list, and the parameterization repeated. All sources
sources detected there may be clumpy gas rather than true              significant at > 4σ in at least one energy band, and within
point sources. To test this, we performed PSF fitting using the         the D25 ellipse of NGC 1672, were retained and visually in-
AE task AE RADIAL PROFILE, which computes a 1-sided                    spected. Spectra, ARFs and RMFs were extracted from the
KS probability to determine whether the observed counts in             data for each source using the SAS task especget.
the 1–2 keV energy range are consistent with the model lo-               The final XMM-Newton catalog contains 19 extra-nuclear
cal 1.49 keV PSF encircled energy distribution. Six candidate          sources, and their properties are listed in Table 1 along with
sources in the ring region were inconsistent with the local PSF        the corresponding Chandra properties. The source fluxes
profile with a significance of > 99%. Sources without detec-             were again determined using spectral fitting (see § 3.3). Note
tions in the hard 2–10 keV band and with a KS probability              that six sources (including the nucleus) within the central
> 99% were deemed to be diffuse and discarded.                         ∼20′′ radius are not spatially resolved with XMM-Newton;
   The final Chandra catalog contains 28 sources inside the             these are marked with (N)=nucleus and (C)=central region
D25 ellipse, and their properties are listed in Table 1. Sources       source. Apart from #10, 17 and 24, all other sources detected
with significance of > 2.5σ were retained, including faint              in the Chandra observation are detected in the XMM-Newton
Chandra counterparts to two significantly detected XMM-                 observation.
Newton sources (for variability and completeness). This
detection threshold corresponds to >12 net source counts.                               3.3. X-ray Source Spectral Fits
Source fluxes were determined using spectral fitting (see
§ 3.3).                                                                   To estimate source fluxes reliably, we have performed spec-
   The absolute astrometry of Chandra is generally accurate            tral fitting on each source using XSPEC v12. Detailed spec-
to within ∼1′′ . 13 To confirm this, the X-ray positions were           tral fitting was performed on Chandra sources with > 100 net
compared to the 2MASS point source catalog. Three coun-                counts, and on XMM-Newton sources with > 100 net counts
terparts were found in the field; the offsets between the X-ray         in either the PN or MOS data. These spectra were binned
and 2MASS positions were small (0.14, 0.16 & 0.6′′ ), and in           (grouped to a minimum of 20 counts per bin) and fitted, using
non-uniform directions, with the greatest offset for a source          χ2 statistics, with both powerlaw+absorption (PO*WABS)
4′ off-axis at the edge of the field. Given this accuracy, no           and disk blackbody+absorption (DISKBB*WABS) models.
astrometric correction was made to the Chandra positions.              In all cases, the powerlaw model provided the best fit. Spec-
                                                                       tral parameters and corresponding 0.3–10 keV fluxes and lu-
               3.2. XMM-Newton Observations                            minosities are shown in Table 1. For the XMM-Newton data,
   NGC 1672 was observed with XMM-Newton for 50 ks on                  the PN, MOS1 and MOS2 spectra were fitted simultaneously.
November 27, 2004 (ObsID 0203880101). The EPIC MOS-                    The fluxes and errors from the three instruments were com-
1, MOS-2 and PN cameras were operated with medium filters               bined to provide a weighted mean flux for each source using
in Prime Full Window mode. Full-field light curves were ac-             the method of Barlow (2004).14
cumulated for the three exposures in the 10–15 keV band to                For sources with < 100 net counts, a simple power-
check for high background intervals of soft proton flares. The          law+Galactic absorption model was fitted to unbinned spec-
data were found to be clean for the duration of the observa-           tra using the C-statistic (Cash 1979). Since at such low
tion, and the full time intervals were used in subsequent anal-        count rates source parameters are difficult to constrain, the
ysis: 47.9 ks (PN), 49.4 ks (MOS1) & 49.5 ks (MOS2). All               powerlaw and absorption parameters were frozen (Γ = 1.7,
    13   http://cxc.harvard.edu/cal/ASPECT/celmon/                       14   http://www.slac.stanford.edu/∼barlow/statistics.html
Investigating the nuclear activity of barred spiral galaxies                                                 5

NHGal = 0.223 × 1021 cm−2 ), with the normalization as the                      An alternative to direct PSF subtraction is to use a nar-
only free parameter. The resulting fluxes and luminosities are                row aperture for the determination of the light within the nu-
also shown in Table 1. The source properties are described in                cleus, and then to apply the aperture corrections tabulated by
§ 4.1.                                                                       Sirianni et al. (2005). We used a 0.1′′ (2 pixel) radius aper-
                                                                             ture, and subtracted the background using an 1.2–2′′ annulus
                      3.4. Multi-wavelength data                             centered on the nucleus. To compare directly with the Chan-
                      3.4.1. HST-ACS Observations                            dra observations, we have also performed photometry using
                                                                             the same physical aperture (1.2′′ radius) and background an-
   NGC 1672 was observed by the Hubble Space Telescope                       nulus (again 1.2–2′′ ). The resulting magnitudes from these
(HST) on August 1, 2005 using the Advanced Camera for                        methods are also shown in Table 2.
Surveys (ACS) Wide Field Channel (WFC) in the broad-                            The upper limits measured using the PSF subtraction
band F435W, F550M and F814W filters, plus the narrow-band                     method are similar to the measurements obtained from the
F658N (Hα) filter. A large dither was implemented, covering                   narrow aperture, though there is a good deal of scatter be-
the dimensions of one of the WFC chips in order to fit the vis-               tween these and the larger Chandra aperture measurements.
ible disk of the galaxy into each observation (see Figure 1).                Given that PSF subtraction gives the most stringent con-
Exposure times were 2444 s in each observation, split into                   straints on the magnitude of a nuclear point source, we adopt
four separate observations corresponding to the visibility of                these limits for the multiwavelength comparison (see Table 3),
NGC 1672 in each single orbit. We also include in our analy-                 and the construction of the nuclear spectral energy distribu-
sis an archival ACS High Resolution Channel (HRC) F330W                      tion (SED, see § 5.2). The AB magnitudes were converted
UV observation of the nucleus of NGC 1672, taken July 19,                    to flux density using ABmag = −2.5 log Fν − 48.6,16 and
2002, with an exposure time of 1140 s. All of the ACS ob-                    then into luminosity using νLν = 4πd2 Fν ×Central filter fre-
servations were processed through the standard multidrizzle                  quency.17 We note that the centroid of the emission in the
pipeline (Koekemoer et al. 2002). As sub-pixel dithers were                  F330W images does not correspond with that seen in data
not used in the observations, the drizzle parameters pixfrac                 taken at longer wavelengths, which suggests that there is some
and scale were set to unity, preserving the native pixel scale of            extinction along the line-of-sight.
both the HRC and WFC. Each of the ACS WFC images were
astrometrically registered with 2MASS stellar objects falling                                      3.4.2. Spitzer IR Observations
within the FOV, yielding an astrometric fit with an RMS of
∼ 0.15′′ . The F658N image is significantly contaminated by                      NGC 1672 was observed with the Spitzer Infrared Ar-
continuum emission within the Hα passband; we therefore                      ray Camera (IRAC, Fazio et al. 2004) on November 29 2006
created a continuum-subtracted image (denoted F658CS) us-                    (Program ID 30496, PI Fisher). Basic Calibrated Data (BCD)
ing a continuum image estimated from a linear combination of                 were retrieved from the archive at 3.6, 4.5, 5.8 and 8.0µm.
the F550M and F814W images (weighted by their separation                     We performed post-BCD processing (mosaicing, with a plate
from the Hα line, and multiplied by the relative sensitivity of              scale of 0.86 arcsec/pixel) using the Spitzer data-processing
each filter to obtain the same physical units in each image).                 package MOPEX (Makovoz et al. 2006). The images are flux
   The ACS images have a very high spatial resolution of                     calibrated in the pipeline in units of surface brightness (MJy
∼0.1′′ . They show that, while the optical emission peaks                    sr−1 ), and we converted them to flux density units by mul-
in the central 2′′ nuclear region, it is clearly non-point like              tiplying by a conversion factor of 1MJy sr−1 = 17.38 µJy
with a FWHM of ∼30 pixels (1.5′′ ). Indeed it displays a                     per pixel. This is a combination of the conversion given in
complex/irregular morphology, and in a visual inspection we                  the Spitzer Observers Manual (1MJy sr−1 = 23.50443 µJy
found no obvious point sources that could correspond to,                     arcsec−2 ), and the pixel solid angle (0.74 arcsec2 ). A MIPS
for example, a nuclear star cluster (which are generally only                (multi-band imaging photometer) 24µm calibrated image was
“marginally resolved ” in HST images of nearby galaxies,                     also retrieved from the archive (from the same Spitzer pro-
B¨ ker et al. 2004). The complexity and extended nature of
  o                                                                          gram), which was reduced using standard pipeline processing.
the region suggests that the use of any moderate sized photo-                A stellar-continuum subtracted 8.0µm (PAH) image was cre-
metric aperture will result in a significant overestimate of the              ated to highlight the star-forming regions, using a conversion
true flux from the nucleus. We investigated this in three ways:               based on a standard model of the starlight near-IR SED; this
(1) via PSF subtraction, (2) narrow aperture photometry, and                 is 8.0µm − 0.232×3.6µm (Helou et al. 2004).
(3) photometry using the Chandra aperture.                                      Photometry was performed on the nuclear source in the four
                                                                                                     ′′
   To estimate the maximum magnitude of any point source at                  IRAC bands using a 1. 5 radius aperture centred on the Chan-
the center of the galaxy, PSFs were constructed from isolated                dra position of the nucleus, using a local annular background
point sources in each image and subtracted from the centroid                 between 2.5–3.0′′. This aperture was chosen because of the
of the galaxy light in each band, scaled such that their cores               larger PSF of IRAC (1.4–1.7′′ FWHM, Fazio et al. 2004), and
resulted in a roughly zero flux value for the brightest pixel                 aperture corrections were applied as detailed in the IRAC
in the galaxy core. For two filters it was not possible to ob-                Data Handbook v3.0, section 5.5.1. The resulting flux den-
tain actual PSFs from the images. In the case of F330W, the                  sities (and AB magnitudes) are shown in Table 3. Note that
HRC field of view is too small for any bright, isolated sources               photometry is not performed on the MIPS data, as the spatial
to be present, while in our F658N continuum-subtracted im-                   resolution (∼6′′ ) is insufficient to separate the nuclear source
age the stars were largely subtracted. To overcome this, we                  from the circumnuclear ring emission.
used TinyTim15 to create artificial PSFs for these filters, which
were then subtracted from the data. The resulting upper limits                                       3.4.3. Radio Observations
are shown in Table 2.
                                                                               16   http://www.stsci.edu/hst/acs/analysis/zeropoints
  15   http://www.stecf.org/instruments/TinyTim/                               17   http://acs.pha.jhu.edu/instrument/filters/general/Master Table.html
6                                                               Jenkins et al.

                          Chandra                                       XMM




                             1’                                (a)         1’                                   (b)

                          Spitzer                                       Chandra
                                                                        (diffuse)




                             1’                                (c)         1’                                   (d)

Figure 2. (a) Chandra 3-color ACIS-S image of NGC 1672: red = 0.3–1 keV, green = 1–2 keV, blue = 2–10 keV. (b) XMM-Newton
EPIC (MOS1+MOS2+PN) 3-color image (in the same energy bands). (c) Spitzer 3-color image: red = 24µm (MIPS), green =
8µm (IRAC), blue = 3.6µm (IRAC). (d) Chandra 3-color image of the diffuse X-ray emission. Contours from the Spitzer IRAC
stellar-continuum-subtracted 8µm data are overlaid, which are spatially correlated with the X-ray emission. The D25 ellipse of
the galaxy is shown with a dashed white line. All images are on the same scale and co-aligned. North is up, east to the left.

   Radio continuum observations of NGC 1672 were ob-                     at 4800 MHz and 4928 MHz, with bandwidths of 128 MHz
tained at 3-cm and 6-cm with the Australia Telescope Com-                divided into 32 channels. At 4864 MHz the ATCA primary
pact Array (ATCA). Data reduction was carried out with the               beam is 9.8′ . The data from both frequency bands were com-
MIRIAD 18 software package, using standard procedures.                   bined, resulting in an angular resolution of 1.9′′ ×1.7′′ and an
   The 3-cm image was created using archival data from a                 rms of 0.04 mJy/beam. The source PKS B1934–638 was used
1.5C configuration obtained in May 2003 and a 6D configura-                as the primary (amplitude & bandpass) calibrator, and PKS
tion obtained in July 2003, with on-source integration times             B0522–611 and PKS B0420–625 were used as the secondary
of 9 h and 10 h respectively. Both observations consist of               (phase) calibrators at 3- and 6-cm, respectively.
two frequency bands centered at 8640 MHz and 8768 MHz,                     A point source fit to the nuclear source gives a position
with bandwidths of 128 MHz divided into 32 channels. At                  of α, δ(J2000) = 04h 45m 42.50s, −59◦ 14′ 49.85′′ (±0.12′′).
8700 MHz the ATCA primary beam is 5.5′ . The data for                    We measure peak fluxes of 0.95 ± 0.15 mJy at 3-cm and
both observations/frequency bands were combined using ‘ro-               1.62±0.15 mJy at 6-cm. We measure integrated flux densities
bust’ weighting (r = 0), resulting in an angular resolution              of 34 mJy (3-cm) and 35 mJy (6-cm) for the radio continuum
of 1.3′′ ×1.0′′ and an rms of 0.03 mJy/beam. The 6-cm im-                emission from both the nuclear source and surrounding star-
age was created using archival data in the 6A configuration               forming ring. It is likely that some extended flux has been
obtained in May 2002, with an on-source integration time of              resolved out by the interferometer. Single-dish radio contin-
11 h. The observation consists of two frequency bands centred            uum flux estimates of NGC 1672 (PMN J0445–5914, PKS
                                                                         J0445–5915) at ∼5 GHz (6-cm) are typically around 100 mJy
    18   http://www.atnf.csiro.au/computing/software/miriad/             (see Wright et al. 1994; Harnett 1987).
Investigating the nuclear activity of barred spiral galaxies                                   7




Figure 3.HST/ACS 3-color image of NGC 1672, produced by Zolt Levay at the Space Telescope Science Institute. The colors
correspond to: red=combined F658N (Hα) + F814W (I), green = F550M (V ), blue = F435W (B). The image is 4.4′ × 3.2′ in
size, with an orientation such that north is 34◦ east (left) of the y-axis.

  There is also one other radio source in the field of view at        detected within the D25 area of the galaxy (blue crosses).
α, δ(J2000) = 04h 45m 36.70s, −59◦ 14′ 28.00′′ (±0.03′′), with       Note that we do not plot the source positions on the HST im-
flux densities of 1.5 ± 0.1 mJy (3-cm) and 1.4 ± 0.1 mJy (6-          age here since it does not cover the entire D25 area. The po-
cm). This is positionally coincident with X-ray source #8            sitions correlate well with the optical structure of the galaxy,
(044536.73–591428.0).                                                with sources concentrated in the nuclear region (see § 4.3) and
                                                                     spread throughout the disk and spiral arms. The extra-nuclear
                         4. RESULTS                                  source fluxes range between FX = 2.3 × 10−15 − 2.8 × 10−13
   Figure 2(a–c) shows 3-color Chandra, XMM-Newton and               erg s−1 cm−2 over both XMM-Newton and Chandra observa-
Spitzer IRAC images of the entire D25 area of NGC 1672.              tions, corresponding to LX = 7.4 × 1037 − 9.0 × 1039 erg
The X-ray sources outside the nuclear region are well re-            s−1 at the distance of NGC 1672.
solved in both the Chandra and XMM-Newton data, and are                 Nine sources, almost a third of the population, reach ul-
discussed in § 4.1. There is also a diffuse hot X-ray gas com-       traluminous X-ray source (ULX) luminosities (LX > 1039
ponent, which is shown in Figure 2(d) as extended red/green          erg s−1 , 0.3–10 keV) in either one or both X-ray observa-
X-ray emission (see § 4.2). The nuclear region is very bright        tions; these are marked with red circles (sources 1, 4, 5, 6,
at all wavelengths, and will be discussed in detail in § 4.3.        7, 13, 24, 25 and 28). Three of the ULXs are very bright
The Spitzer IR data show that the majority of the non-nuclear        (sources 4, 5, and 25 with LX > 5 × 1039 erg s−1 , marked
star-formation activity is confined to the bar and inner spiral       with larger circles), and are co-spatial with the ends of the
arms (illustrated in red and green), whereas older stellar pop-      bar (as previously noted by Brandt et al. 1996). This is con-
ulations are spread throughout the disk (illustrated in blue).       sistent with models that show that gas can accumulate at the
Figure 3 shows the high-resolution 3-color HST/ACS image,            tips of bars due to the corotation of the bar structure with
where the bar structure, numerous HII regions and dust lanes         the disk (Englmaier & Gerhard 1997), thereby creating star-
are visible.                                                         forming regions where X-ray binaries can form. Other exam-
                                                                     ples of this phenomenon have been observed in the barred
             4.1. X-ray Point Source Population                      galaxies NGC 7771 (Jenkins et al. 2005) and NGC 4303
                                                                     (Jim´ nez-Bail´ n et al. 2003).
                                                                          e         o
 Figure 4 (top left) shows the DSS optical image of
                                                                        Figure 4 (top right) shows the source positions overlaid on
NGC 1672, overlaid with the positions of the 28 X-ray sources
8                                                             Jenkins et al.

               DSS                                                    Spitzer                                   8µm




                    1’                                                     1’

                                 s26                                  s8




Figure 4.Top left: DSS optical image of NGC1672 with the 28 X-ray source positions marked with blue crosses. Sources with
LX > 1039 erg s−1 in the 0.3–10 keV band (i.e. ULXs) in either the XMM-Newton or Chandra observation are marked with red
circles, with the 3 brightest (LX > 5 × 1039 erg s−1 ) denoted by larger circles (#4, 5 & 25). Sources that show variability of
> 2.5σ between the two observations are also marked with white squares (including sources detected in only one observation).
The dotted diamonds denote sources #8 & 26, which are resolved as background galaxies in the optical HST/ACS images; these
are shown in the lower panel, where the diamond boxes are 2′′ × 2′′ centered on the X-ray positions. Top right: the Spitzer IRAC
continuum-subtracted 8µm image, showing the locations of the X-ray sources with respect to star-forming regions in the galaxy.

the Spitzer 8µm image, illustrating the coincidence of many               Figure 4 (top left) also denotes variable sources (marked
X-ray sources with regions of star-formation in the bar and            with white squares). Six sources show significant long-term
inner spiral arm regions. We have correlated the X-ray source          flux variability between the XMM-Newton and Chandra ob-
positions with the HII region catalog of Evans et al. (1996).          servations at levels of > 2.5σ; these are sources 1, 4, 6, 8, 21
Taking into account both the absolute astrometric accuracy of          and 25. Most notable are the increases in flux in two of the
the X-ray and HII region positions (∼1′′ combined) as well as          brightest ULXs in the Chandra observations; #4 increases by
the measured areas of the HII regions, we associate eleven X-          a factor of ∼5 (up to 6.9 × 1039 erg s−1 ), and #25 increases
ray sources with HII regions (2, 4, 5, 7, 13, 14, 18, 21, 25, 27,      by a factor of ∼3 (up to 9.0 × 1039 erg s−1 ), indicating that
and 28). These include the three brightest ULXs, and three             the high luminosity of these sources is not due to confusion
sources in the circumnuclear ring.                                     of several fainter sources. These flux increases are accompa-
  We have not performed any complex spectral fitting on the             nied by a spectral hardening of source #4, but no significant
X-ray sources, as even the brightest are well-fit with simple           spectral change in source #25. The other four sources with
                                         2
absorption+powerlaw models, with χν close to 1 (see Ta-                spectral fits in both observations show no significant spectral
ble 1). The spectra and model fits are shown in Figures 5               change between observations. Another four sources (10, 17,
and 6. However, we note that even though this simple model             24 and 27) are only detected in one observation.
provides acceptable empirical fits to these data, this is likely           To investigate longer-term behavior, in Table 4 we show
due to the relatively low photon counts ( 2000 counts, total           a comparison between XMM-Newton, Chandra and ROSAT
PN+MOS or ACIS-S), and the true underlying spectral shapes             HRI soft X-ray luminosities for five sources detected in
are likely to be more complex (see Stobbart et al. 2006 for a          all three observations. We quote the 0.2–2 keV HRI lu-
discussion).                                                           minosities from de Naray et al. (2000) for the combined
Investigating the nuclear activity of barred spiral galaxies                                                                                                                                                                                                                                                9
 Normalization (count s−1 keV−1)




                                                                                                                                            Normalization (count s−1 keV−1)




                                                                                                                                                                                                                                                                                                                           Normalization (count s−1 keV−1)
                                                                                                                                                                              0.01
                                                                                                                                 S1                                                                                                                                                                             S4                                                                                                               S5
                                   2×10−4 5×10−4 10−3 2×10−3




                                                                                                                                                                                                                                                                                                                                                             0.01
                                                                                                                                                                              10−3




                                                                                                                                                                                                                                                                                                                                                             10−3
                                                                                                                                                                              10−4




                                                                                                                                                                                                                                                                                                                                                             1.5
                                   1.5




                                                                                                                                                                              1.5
 Ratio




                                                                                                                                            Ratio




                                                                                                                                                                                                                                                                                                                           Ratio
                                                                                                                                                                                                                                                                                                                                                             1
                                   1




                                                                                                                                                                              1
                                                               0.5   1           2                                          5          10                                                                       0.5        1            2                                                                   5         10                                                                      0.5        1            2      5         10
                                                                         Energy (keV)                                                                                                                                           Energy (keV)                                                                                                                                                                  Energy (keV)




                                                                                                                                                                              2×10−4 5×10−4 10−32×10−3 5×10−3
 Normalization (count s−1 keV−1)




                                                                                                                                                                                                                                                                                                                           Normalization (count s−1 keV−1)
                                                                                                                                            Normalization (count s−1 keV−1)
                                                                                                                                 S6                                                                                                                                                                             S7                                                                                                               S19
                                   5×10−4 10−3 2×10−3




                                                                                                                                                                                                                                                                                                                                                             10−3
                                                                                                                                                                                                                                                                                                                                                             10−4
                                   2×10−4




                                                                                                                                                                                                                                                                                                                                                             2
                                   1.5




                                                                                                                                                                              1.5




                                                                                                                                                                                                                                                                                                                                                             1.5
 Ratio




                                                                                                                                                                                                                                                                                                                           Ratio
                                                                                                                                            Ratio
                                   1




                                                                                                                                                                              1




                                                                                                                                                                                                                                                                                                                                                             1
                                                               0.5   1           2                                          5          10                                                                       0.5        1            2                                                                   5         10                                                                      0.5        1            2      5         10
                                                                         Energy (keV)                                                                                                                                           Energy (keV)                                                                                                                                                                  Energy (keV)




                                                                                                                                                                                                                                                                                                                                                             10−4 2×10−4 5×10−4 10−3 2×10−3
 Normalization (count s−1 keV−1)




                                                                                                                                            Normalization (count s−1 keV−1)




                                                                                                                                                                                                                                                                                                                           Normalization (count s−1 keV−1)
                                                                                                                                 S22                                                                                                                                                                            S25
                                                                                                                                                                              0.01




                                                                                                                                                                                                                                                                                                                                                                                                                                 S26
                                   10−3




                                                                                                                                                                              10−3
                                   10−4




                                                                                                                                                                              10−4
                                                                                                                                                                              1.5
                                   1.5




                                                                                                                                                                                                                                                                                                                                                             1.5
 Ratio




                                                                                                                                            Ratio




                                                                                                                                                                                                                                                                                                                           Ratio
                                                                                                                                                                              1
                                   1




                                                                                                                                                                                                                                                                                                                                                             1
                                                                                                                                                                              0.5




                                                               0.5   1           2                                          5          10                                                                       0.5        1            2                                                                   5         10
                                                                         Energy (keV)                                                                                                                                           Energy (keV)                                                                                                                                                  0.5        1            2      5         10
                                                                                                                                                                                                                                                                                                                                                                                                              Energy (keV)
                                                                             Normalization (count s−1 keV−1)




                                                                                                                                                                                                                                     Normalization (count s−1 keV−1)
                                                                                                                                                                                                                                                                       10−42×10−4 5×10−4 10−32×10−3




                                                                                                                                                                                                                          S27                                                                                                                                                                           S28
                                                                                                               10−3
                                                                                                               10−4
                                                                                                               1.5




                                                                                                                                                                                                                                                                       1.5
                                                                             Ratio




                                                                                                                                                                                                                                     Ratio
                                                                                                               1




                                                                                                                                                                                                                                                                       1




                                                                                                                      0.5          1           2                                                                      5         10                                                                    0.5        1            2                                                                     5         10
                                                                                                                                       Energy (keV)                                                                                                                                                                   Energy (keV)


       XMM-Newton EPIC spectra of the 11 sources with > 100 net PN or MOS counts. PN data points and power-
Figure 5.
law+absorption models are shown in green; those of the MOS data are shown in red/black.

1992/1997 dataset (which gives better photon statistics), to-                                                                                                                                                                                                                            We estimate the number of background X-ray sources in the
gether with 0.2–2 keV luminosities derived from the best-                                                                                                                                                                                                                             D25 area of NGC 1672 using the hard-band (2–10 keV) log
fit XMM-Newton and Chandra spectral models corrected for                                                                                                                                                                                                                               N -log S source distributions from Chandra deep field studies
Galactic absorption. Note that we also include #23 (ROSAT                                                                                                                                                                                                                             (we do not use the soft-band log N -log S since the detec-
source X-5), which was originally believed to be coincident                                                                                                                                                                                                                           tion sensitivity at soft energies will be affected by absorption
with a foreground star given the ROSAT positional errors                                                                                                                                                                                                                              by neutral material in the galactic disk). Using a source de-
(∼5′′ ). However, with the Chandra positional accuracy of                                                                                                                                                                                                                             tection threshold of 12 counts in the 0.3–10 keV band (corre-
∼0.5′′ , we show that this source is not consistent with the                                                                                                                                                                                                                          sponding to the faintest source detected in the Chandra ob-
2MASS position of the star (04h 45m49.54s , −59◦12′ 54.1′′)                                                                                                                                                                                                                           servation), and converting this to a 2–10 keV flux for a typi-
with an offset of ∼5′′ . In fact, this is the source that shows the                                                                                                                                                                                                                   cal AGN (∼ 1.5 × 10−15 erg s−1 cm−2 , using Γ = 1.7 and
largest long-term variability with Lhigh /Llow = 3.6 over this                                                                                                                                                                                                                        NHGal = 0.223 × 1021 cm−2 ), the log N -log S relations of
∼10 year period. The remaining sources vary in luminosity                                                                                                                                                                                                                             Giacconi et al. (2001), Campana et al. (2001) and Bauer et al.
by factors of 1 − 3.                                                                                                                                                                                                                                                                  (2004) all predict between 2–3 background sources in the
10                                                                                                                                                                                                   Jenkins et al.




                                                                                                                                                                                                                                                                                                                       5×10−4 10−3 2×10−3 5×10−3 0.01 0.02
                                                                                                                                                         10−3 2×10−3 5×10−3 0.01 0.02
 Normalization (count s−1 keV−1)




                                                                                                                       Normalization (count s−1 keV−1)




                                                                                                                                                                                                                                                                                     Normalization (count s−1 keV−1)
                                                                                                             S1                                                                                                                                                           S4
                                   10−3

                                                                                                                                                                                                                                                                                                                                                                                                S5
                                   5×10−4
                                   2×10−4
                                   1.5




                                                                                                                                                         1.5




                                                                                                                                                                                                                                                                                                                       1.5
 Ratio




                                                                                                                       Ratio




                                                                                                                                                                                                                                                                                     Ratio
                                   1




                                                                                                                                                         1




                                                                                                                                                                                                                                                                                                                       1
                                            0.5   1           2                                          5        10                                                                      0.5        1            2                                                   5         10
                                                      Energy (keV)                                                                                                                                        Energy (keV)                                                                                                                                       0.5        1            2      5         10
                                                                                                                                                                                                                                                                                                                                                                             Energy (keV)




                                                                                                                                                         5×10−4 10−3 2×10−3 5×10−3 0.01




                                                                                                                                                                                                                                                                                                                       2×10−4 5×10−4 10−32×10−3 5×10−3
                                   2×10−3
 Normalization (count s−1 keV−1)




                                                                                                                       Normalization (count s−1 keV−1)




                                                                                                                                                                                                                                                                                     Normalization (count s−1 keV−1)
                                                                                                             S7                                                                                                                                                           S13
                                                                                                                                                                                                                                                                                                                                                                                                S24
                                   10−3
                                   5×10−4
                                   1.5




                                                                                                                                                         1.5




                                                                                                                                                                                                                                                                                                                       1.5
 Ratio




                                                                                                                       Ratio




                                                                                                                                                                                                                                                                                     Ratio
                                   1




                                                                                                                                                         1




                                                                                                                                                                                                                                                                                                                       1
                                            0.5   1           2                                          5        10                                                                      0.5        1            2                                                   5         10
                                                      Energy (keV)                                                                                                                                        Energy (keV)                                                                                                                                       0.5        1            2      5         10
                                                                                                                                                                                                                                                                                                                                                                             Energy (keV)
                                                          Normalization (count s−1 keV−1)




                                                                                                                                                                                                               Normalization (count s−1 keV−1)
                                                                                                                                                                                                                                                 2×10−3
                                                                                                                                                                                                    S25                                                                                                                                                                S28
                                                                                            0.01




                                                                                                                                                                                                                                                 10−3
                                                                                            10−3




                                                                                                                                                                                                                                                 5×10−4
                                                                                                                                                                                                                                                 1.5
                                                                                            1.5
                                                          Ratio




                                                                                                                                                                                                               Ratio
                                                                                                                                                                                                                                                 1
                                                                                            1




                                                                                                   0.5        1           2                                                                     5         10                                                    0.5        1            2                                                                          5         10
                                                                                                                  Energy (keV)                                                                                                                                                  Energy (keV)


                                   Figure 6. Chandra ACIS-S                                        spectra of the 8 sources with > 100 net counts, together with the powerlaw+absorption models.

field. Note that this is in fact an upper limit, since the                                                                                                                                                                                           contours from the continuum-subtracted Spitzer IRAC 8.0µm
NGC 1672 source catalog is not corrected for incompleteness.                                                                                                                                                                                        image, which highlights star-formation activity; the diffuse
Inspection of the HST/ACS images allows us to identify two                                                                                                                                                                                          emission is spatially correlated with the IR emission, follow-
X-ray sources as background galaxies immediately; these are                                                                                                                                                                                         ing the bar/inner spiral arm structure.
#26, which appears to be a face-on disk galaxy with a bright                                                                                                                                                                                           A source spectrum was extracted from an elliptical region
nucleus, and #8, which looks like an edge-on galaxy with vis-                                                                                                                                                                                       (a, b) = (2.25′ , 1.11′ ) centered on the nucleus with a posi-
ible dust lanes seen through the disk of NGC 1672 (see Fig-                                                                                                                                                                                         tion angle of 90◦ . The detected point sources were excluded
ure 4, lower panel). As noted in § 3.4.3, source #8 is the only                                                                                                                                                                                     (using regions with twice the radius of the 90% encircled en-
extra-nuclear X-ray source with a detected radio counterpart.                                                                                                                                                                                       ergy ellipses), as well as the innermost 20′′ radius circumnu-
At the distance of NGC 1672, the 2–10 keV X-ray luminos-                                                                                                                                                                                            clear ring region. The background regions were chosen to be
ity (at its brightest in the XMM-Newton observation) would                                                                                                                                                                                          (1) the region on the ACIS-S3 chip outside the D25 radius
be LX = 7.9 × 1038 erg s−1 , and the 5 GHz radio luminosity                                                                                                                                                                                         and not containing point sources, and (2) the region on the
would be νLν = 2.2 × 1036 erg s−1 . According to the X-                                                                                                                                                                                             ACIS-S1 chip not containing bright point sources. To further
ray/radio fundamental plane of Merloni et al. (2003), this is                                                                                                                                                                                       constrain the soft end of the background emission, we also
inconsistent with emission from a stellar mass black hole (i.e.                                                                                                                                                                                     used the seven element ROSAT All Sky Survey (RASS) spec-
too radio-bright), and supports the hypothesis that this source                                                                                                                                                                                     tral energy distribution (Snowden et al. 1997) from an annulus
is a background AGN (see § 5 for further discussion of this                                                                                                                                                                                         30′ < R < 1◦ around NGC 1672, extracted using the X-ray
relation with regards to the nuclear source).                                                                                                                                                                                                       background web tool hosted by the HEASARC19 . For each
                                                                                                                                                                                                                                                    Chandra spectrum, we created a particle background spec-
                 4.2. Diffuse X-ray Emission
                                                                                                                                                                                                                                                    trum using the “stowed” data from the appropriate chip and
   We have used the Chandra observation to study the diffuse                                                                                                                                                                                        mode, scaled to produce the same 10–13 keV band count rate
X-ray component of NGC 1672 due to its ∼1′′ spatial resolu-                                                                                                                                                                                         as observed in the ObsID 5932 data. The particle background
tion, and hence ease of source subtraction. The morphology                                                                                                                                                                                          spectra were then used as the “background” spectra within
of the diffuse emission is illustrated in Figure 2 (d), where the                                                                                                                                                                                   XSPEC, and the spectra of the galaxy and the remainder of the
X-ray point sources and central ring region have been masked,
                                                                                                                                                                                                                                                          19   http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/xraybg/xraybg.pl
and the residual emission adaptively smoothed. Overlaid are
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672
Investigating the nuclear_activity_of_ngc1672

Weitere ähnliche Inhalte

Was ist angesagt?

Star formation history_in_the_smc_the_case_of_ngc602
Star formation history_in_the_smc_the_case_of_ngc602Star formation history_in_the_smc_the_case_of_ngc602
Star formation history_in_the_smc_the_case_of_ngc602Sérgio Sacani
 
First detection of_molecular_gas_in_shells_in_cena_galaxy
First detection of_molecular_gas_in_shells_in_cena_galaxyFirst detection of_molecular_gas_in_shells_in_cena_galaxy
First detection of_molecular_gas_in_shells_in_cena_galaxySérgio Sacani
 
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...Sérgio Sacani
 
Kepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planet
Kepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planetKepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planet
Kepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planetSérgio Sacani
 
Creation of cosmic structure in the complex galaxy cluster merger abell 2744
Creation of cosmic structure in the complex galaxy cluster  merger abell 2744Creation of cosmic structure in the complex galaxy cluster  merger abell 2744
Creation of cosmic structure in the complex galaxy cluster merger abell 2744Sérgio Sacani
 
Shaping the glowing_eye_planetary_nebula_ngc6751
Shaping the glowing_eye_planetary_nebula_ngc6751Shaping the glowing_eye_planetary_nebula_ngc6751
Shaping the glowing_eye_planetary_nebula_ngc6751Sérgio Sacani
 
Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...
Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...
Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...Sérgio Sacani
 
Too much pasta_for_pulsars_to_spin_down
Too much pasta_for_pulsars_to_spin_downToo much pasta_for_pulsars_to_spin_down
Too much pasta_for_pulsars_to_spin_downSérgio Sacani
 
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...Sérgio Sacani
 
Multi wavelenth observations and surveys of galaxy clusters
Multi wavelenth observations and surveys of galaxy clustersMulti wavelenth observations and surveys of galaxy clusters
Multi wavelenth observations and surveys of galaxy clustersJoana Santos
 
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001ig
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001igModulations in the_radio_light_curve_of_the_typeiib_supernova_2001ig
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001igSérgio Sacani
 
A new spin_of_the_first_stars
A new spin_of_the_first_starsA new spin_of_the_first_stars
A new spin_of_the_first_starsSérgio Sacani
 
Origin of the fermi bubble
Origin of the fermi bubbleOrigin of the fermi bubble
Origin of the fermi bubbleSérgio Sacani
 
Relativistic collapse and explosion of rotating supermassive stars with therm...
Relativistic collapse and explosion of rotating supermassive stars with therm...Relativistic collapse and explosion of rotating supermassive stars with therm...
Relativistic collapse and explosion of rotating supermassive stars with therm...Sérgio Sacani
 
Type iax supernovae_a_new_class_of_stellar_explosion
Type iax supernovae_a_new_class_of_stellar_explosionType iax supernovae_a_new_class_of_stellar_explosion
Type iax supernovae_a_new_class_of_stellar_explosionSérgio Sacani
 
Deep nearinfrared survey_carina_nebula
Deep nearinfrared survey_carina_nebulaDeep nearinfrared survey_carina_nebula
Deep nearinfrared survey_carina_nebulaSérgio Sacani
 
Salts and radiation_products_on_the_surface_of_europa
Salts and radiation_products_on_the_surface_of_europaSalts and radiation_products_on_the_surface_of_europa
Salts and radiation_products_on_the_surface_of_europaSérgio Sacani
 
Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...
Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...
Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...Sérgio Sacani
 
Methane ethane on_the_bright_kuiper_belt_object_2005_fy9
Methane ethane on_the_bright_kuiper_belt_object_2005_fy9Methane ethane on_the_bright_kuiper_belt_object_2005_fy9
Methane ethane on_the_bright_kuiper_belt_object_2005_fy9Sérgio Sacani
 
Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...
Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...
Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...Sérgio Sacani
 

Was ist angesagt? (20)

Star formation history_in_the_smc_the_case_of_ngc602
Star formation history_in_the_smc_the_case_of_ngc602Star formation history_in_the_smc_the_case_of_ngc602
Star formation history_in_the_smc_the_case_of_ngc602
 
First detection of_molecular_gas_in_shells_in_cena_galaxy
First detection of_molecular_gas_in_shells_in_cena_galaxyFirst detection of_molecular_gas_in_shells_in_cena_galaxy
First detection of_molecular_gas_in_shells_in_cena_galaxy
 
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...
 
Kepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planet
Kepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planetKepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planet
Kepler 413b a_slightly_misaligned_neptune_size_transiting_circumbinary_planet
 
Creation of cosmic structure in the complex galaxy cluster merger abell 2744
Creation of cosmic structure in the complex galaxy cluster  merger abell 2744Creation of cosmic structure in the complex galaxy cluster  merger abell 2744
Creation of cosmic structure in the complex galaxy cluster merger abell 2744
 
Shaping the glowing_eye_planetary_nebula_ngc6751
Shaping the glowing_eye_planetary_nebula_ngc6751Shaping the glowing_eye_planetary_nebula_ngc6751
Shaping the glowing_eye_planetary_nebula_ngc6751
 
Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...
Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...
Hst imaging of_fading_agn_candidates_i_host_galaxy_properties_and_origin_of_t...
 
Too much pasta_for_pulsars_to_spin_down
Too much pasta_for_pulsars_to_spin_downToo much pasta_for_pulsars_to_spin_down
Too much pasta_for_pulsars_to_spin_down
 
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...
 
Multi wavelenth observations and surveys of galaxy clusters
Multi wavelenth observations and surveys of galaxy clustersMulti wavelenth observations and surveys of galaxy clusters
Multi wavelenth observations and surveys of galaxy clusters
 
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001ig
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001igModulations in the_radio_light_curve_of_the_typeiib_supernova_2001ig
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001ig
 
A new spin_of_the_first_stars
A new spin_of_the_first_starsA new spin_of_the_first_stars
A new spin_of_the_first_stars
 
Origin of the fermi bubble
Origin of the fermi bubbleOrigin of the fermi bubble
Origin of the fermi bubble
 
Relativistic collapse and explosion of rotating supermassive stars with therm...
Relativistic collapse and explosion of rotating supermassive stars with therm...Relativistic collapse and explosion of rotating supermassive stars with therm...
Relativistic collapse and explosion of rotating supermassive stars with therm...
 
Type iax supernovae_a_new_class_of_stellar_explosion
Type iax supernovae_a_new_class_of_stellar_explosionType iax supernovae_a_new_class_of_stellar_explosion
Type iax supernovae_a_new_class_of_stellar_explosion
 
Deep nearinfrared survey_carina_nebula
Deep nearinfrared survey_carina_nebulaDeep nearinfrared survey_carina_nebula
Deep nearinfrared survey_carina_nebula
 
Salts and radiation_products_on_the_surface_of_europa
Salts and radiation_products_on_the_surface_of_europaSalts and radiation_products_on_the_surface_of_europa
Salts and radiation_products_on_the_surface_of_europa
 
Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...
Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...
Shock breakout and_early_light_curves_of_type_ii_p_supernovae_observed_with_k...
 
Methane ethane on_the_bright_kuiper_belt_object_2005_fy9
Methane ethane on_the_bright_kuiper_belt_object_2005_fy9Methane ethane on_the_bright_kuiper_belt_object_2005_fy9
Methane ethane on_the_bright_kuiper_belt_object_2005_fy9
 
Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...
Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...
Precision measurement of_the_most_distant_spectroscopically_confirmed_superno...
 

Andere mochten auch

5 July in Pictures -- Women's Worlds 2011
5 July in Pictures -- Women's Worlds 20115 July in Pictures -- Women's Worlds 2011
5 July in Pictures -- Women's Worlds 2011Women's Worlds 2011
 
1 July in pictures -- Women's Worlds 2011
1 July in pictures -- Women's Worlds 20111 July in pictures -- Women's Worlds 2011
1 July in pictures -- Women's Worlds 2011Women's Worlds 2011
 
Urbanismo emergente (paisajes domesticos 2009)
Urbanismo emergente (paisajes domesticos 2009)Urbanismo emergente (paisajes domesticos 2009)
Urbanismo emergente (paisajes domesticos 2009)Sebastian Bernal Franco
 
WW 2011 general overview may2010
WW 2011 general overview may2010WW 2011 general overview may2010
WW 2011 general overview may2010Women's Worlds 2011
 
2/3 July in pictures -- Women's Worlds 2011
2/3 July in pictures -- Women's Worlds 20112/3 July in pictures -- Women's Worlds 2011
2/3 July in pictures -- Women's Worlds 2011Women's Worlds 2011
 
Social business systems - success factors for Enterprise 2.0 applications
Social business systems - success factors for Enterprise 2.0 applicationsSocial business systems - success factors for Enterprise 2.0 applications
Social business systems - success factors for Enterprise 2.0 applicationsHuddleHQ
 
The close circumstellar environment of betelgeuse
The close circumstellar environment of betelgeuseThe close circumstellar environment of betelgeuse
The close circumstellar environment of betelgeuseSérgio Sacani
 
Kepler 34 b_e_kepler_35_b
Kepler 34 b_e_kepler_35_bKepler 34 b_e_kepler_35_b
Kepler 34 b_e_kepler_35_bSérgio Sacani
 
Amigounminuto
AmigounminutoAmigounminuto
Amigounminutolehike
 
Science 2011-akeson-316-7
Science 2011-akeson-316-7Science 2011-akeson-316-7
Science 2011-akeson-316-7Sérgio Sacani
 
Likes health project
Likes   health projectLikes   health project
Likes health projectmschlafly
 
4 July in pictures -- Women's Worlds 2011
4 July in pictures -- Women's Worlds 20114 July in pictures -- Women's Worlds 2011
4 July in pictures -- Women's Worlds 2011Women's Worlds 2011
 
OverDrive & mobile technology
OverDrive & mobile technologyOverDrive & mobile technology
OverDrive & mobile technologyguest44e9eeb
 
Cesc 2010 Slide Show New Employee
Cesc 2010 Slide Show   New EmployeeCesc 2010 Slide Show   New Employee
Cesc 2010 Slide Show New EmployeeJames Jolly
 

Andere mochten auch (18)

5 July in Pictures -- Women's Worlds 2011
5 July in Pictures -- Women's Worlds 20115 July in Pictures -- Women's Worlds 2011
5 July in Pictures -- Women's Worlds 2011
 
1 July in pictures -- Women's Worlds 2011
1 July in pictures -- Women's Worlds 20111 July in pictures -- Women's Worlds 2011
1 July in pictures -- Women's Worlds 2011
 
Urbanismo emergente (paisajes domesticos 2009)
Urbanismo emergente (paisajes domesticos 2009)Urbanismo emergente (paisajes domesticos 2009)
Urbanismo emergente (paisajes domesticos 2009)
 
WW 2011 general overview may2010
WW 2011 general overview may2010WW 2011 general overview may2010
WW 2011 general overview may2010
 
2/3 July in pictures -- Women's Worlds 2011
2/3 July in pictures -- Women's Worlds 20112/3 July in pictures -- Women's Worlds 2011
2/3 July in pictures -- Women's Worlds 2011
 
WW 2011 is out there
WW 2011 is out thereWW 2011 is out there
WW 2011 is out there
 
Social business systems - success factors for Enterprise 2.0 applications
Social business systems - success factors for Enterprise 2.0 applicationsSocial business systems - success factors for Enterprise 2.0 applications
Social business systems - success factors for Enterprise 2.0 applications
 
The close circumstellar environment of betelgeuse
The close circumstellar environment of betelgeuseThe close circumstellar environment of betelgeuse
The close circumstellar environment of betelgeuse
 
Kepler 34 b_e_kepler_35_b
Kepler 34 b_e_kepler_35_bKepler 34 b_e_kepler_35_b
Kepler 34 b_e_kepler_35_b
 
Amigounminuto
AmigounminutoAmigounminuto
Amigounminuto
 
Science 2011-akeson-316-7
Science 2011-akeson-316-7Science 2011-akeson-316-7
Science 2011-akeson-316-7
 
Likes health project
Likes   health projectLikes   health project
Likes health project
 
4 July in pictures -- Women's Worlds 2011
4 July in pictures -- Women's Worlds 20114 July in pictures -- Women's Worlds 2011
4 July in pictures -- Women's Worlds 2011
 
Imágenes ppt
Imágenes pptImágenes ppt
Imágenes ppt
 
OverDrive & mobile technology
OverDrive & mobile technologyOverDrive & mobile technology
OverDrive & mobile technology
 
Cesc 2010 Slide Show New Employee
Cesc 2010 Slide Show   New EmployeeCesc 2010 Slide Show   New Employee
Cesc 2010 Slide Show New Employee
 
Eco fashion
Eco fashionEco fashion
Eco fashion
 
7 July in Pictures
7 July in Pictures7 July in Pictures
7 July in Pictures
 

Ähnlich wie Investigating the nuclear_activity_of_ngc1672

Ngc3801 caught in_the_act_a_post_merger_starforming
Ngc3801 caught in_the_act_a_post_merger_starformingNgc3801 caught in_the_act_a_post_merger_starforming
Ngc3801 caught in_the_act_a_post_merger_starformingSérgio Sacani
 
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...Sérgio Sacani
 
Alma observations of_feed_and_feedback_in_nearby_seyfert_galaxies
Alma observations of_feed_and_feedback_in_nearby_seyfert_galaxiesAlma observations of_feed_and_feedback_in_nearby_seyfert_galaxies
Alma observations of_feed_and_feedback_in_nearby_seyfert_galaxiesSérgio Sacani
 
An exceptional xray_view_of_the_young_open_cluster_ngc6231
An exceptional xray_view_of_the_young_open_cluster_ngc6231An exceptional xray_view_of_the_young_open_cluster_ngc6231
An exceptional xray_view_of_the_young_open_cluster_ngc6231Sérgio Sacani
 
Three newly discovered_globular_clusters_in_ngc6822
Three newly discovered_globular_clusters_in_ngc6822Three newly discovered_globular_clusters_in_ngc6822
Three newly discovered_globular_clusters_in_ngc6822Sérgio Sacani
 
Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...
Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...
Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...Sérgio Sacani
 
The extended optical_disk_of_m101
The extended optical_disk_of_m101The extended optical_disk_of_m101
The extended optical_disk_of_m101Sérgio Sacani
 
Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...
Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...
Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...Sérgio Sacani
 
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...Sérgio Sacani
 
Formation of polar_ring_galaxies
Formation of polar_ring_galaxiesFormation of polar_ring_galaxies
Formation of polar_ring_galaxiesSérgio Sacani
 
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...Sérgio Sacani
 
A multiband study_of_hercules_a_ii_multifrequency_vla
A multiband study_of_hercules_a_ii_multifrequency_vlaA multiband study_of_hercules_a_ii_multifrequency_vla
A multiband study_of_hercules_a_ii_multifrequency_vlaSérgio Sacani
 
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068Sérgio Sacani
 
Galaxies. Quasars. lecture notes chapter 20
Galaxies. Quasars. lecture notes chapter 20Galaxies. Quasars. lecture notes chapter 20
Galaxies. Quasars. lecture notes chapter 20Lionel Wolberger
 

Ähnlich wie Investigating the nuclear_activity_of_ngc1672 (20)

Ngc3801 caught in_the_act_a_post_merger_starforming
Ngc3801 caught in_the_act_a_post_merger_starformingNgc3801 caught in_the_act_a_post_merger_starforming
Ngc3801 caught in_the_act_a_post_merger_starforming
 
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...
 
Alma observations of_feed_and_feedback_in_nearby_seyfert_galaxies
Alma observations of_feed_and_feedback_in_nearby_seyfert_galaxiesAlma observations of_feed_and_feedback_in_nearby_seyfert_galaxies
Alma observations of_feed_and_feedback_in_nearby_seyfert_galaxies
 
An exceptional xray_view_of_the_young_open_cluster_ngc6231
An exceptional xray_view_of_the_young_open_cluster_ngc6231An exceptional xray_view_of_the_young_open_cluster_ngc6231
An exceptional xray_view_of_the_young_open_cluster_ngc6231
 
Three newly discovered_globular_clusters_in_ngc6822
Three newly discovered_globular_clusters_in_ngc6822Three newly discovered_globular_clusters_in_ngc6822
Three newly discovered_globular_clusters_in_ngc6822
 
Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...
Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...
Catch me if_you_can_is_there_a_runaway_mass_black_hole_in_the_orion_nebula_cl...
 
The extended optical_disk_of_m101
The extended optical_disk_of_m101The extended optical_disk_of_m101
The extended optical_disk_of_m101
 
Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...
Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...
Asymmetrical structure of_ionization_and_kinematics_in_the_seyfert_galaxy_ngc...
 
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...
 
Formation of polar_ring_galaxies
Formation of polar_ring_galaxiesFormation of polar_ring_galaxies
Formation of polar_ring_galaxies
 
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...
Asymmetrical tidal tails of open star clusters: stars crossing their cluster’...
 
A multiband study_of_hercules_a_ii_multifrequency_vla
A multiband study_of_hercules_a_ii_multifrequency_vlaA multiband study_of_hercules_a_ii_multifrequency_vla
A multiband study_of_hercules_a_ii_multifrequency_vla
 
Ngc760 02
Ngc760 02Ngc760 02
Ngc760 02
 
Ngc 4151 02
Ngc 4151 02Ngc 4151 02
Ngc 4151 02
 
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068
Solving the Multimessenger Puzzle of the AGN-starburst Composite Galaxy NGC 1068
 
1212.1169
1212.11691212.1169
1212.1169
 
Karavasilev
KaravasilevKaravasilev
Karavasilev
 
Karavasilev
KaravasilevKaravasilev
Karavasilev
 
Ngc 4151 03
Ngc 4151 03Ngc 4151 03
Ngc 4151 03
 
Galaxies. Quasars. lecture notes chapter 20
Galaxies. Quasars. lecture notes chapter 20Galaxies. Quasars. lecture notes chapter 20
Galaxies. Quasars. lecture notes chapter 20
 

Mehr von Sérgio Sacani

Thermonuclear explosions on neutron stars reveal the speed of their jets
Thermonuclear explosions on neutron stars reveal the speed of their jetsThermonuclear explosions on neutron stars reveal the speed of their jets
Thermonuclear explosions on neutron stars reveal the speed of their jetsSérgio Sacani
 
Identification of Superclusters and Their Properties in the Sloan Digital Sky...
Identification of Superclusters and Their Properties in the Sloan Digital Sky...Identification of Superclusters and Their Properties in the Sloan Digital Sky...
Identification of Superclusters and Their Properties in the Sloan Digital Sky...Sérgio Sacani
 
Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...
Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...
Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...Sérgio Sacani
 
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky Way
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky WayShiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky Way
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky WaySérgio Sacani
 
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...Sérgio Sacani
 
Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...
Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...
Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...Sérgio Sacani
 
Revelando Marte - Livro Sobre a Exploração do Planeta Vermelho
Revelando Marte - Livro Sobre a Exploração do Planeta VermelhoRevelando Marte - Livro Sobre a Exploração do Planeta Vermelho
Revelando Marte - Livro Sobre a Exploração do Planeta VermelhoSérgio Sacani
 
Weak-lensing detection of intracluster filaments in the Coma cluster
Weak-lensing detection of intracluster filaments in the Coma clusterWeak-lensing detection of intracluster filaments in the Coma cluster
Weak-lensing detection of intracluster filaments in the Coma clusterSérgio Sacani
 
Quasar and Microquasar Series - Microquasars in our Galaxy
Quasar and Microquasar Series - Microquasars in our GalaxyQuasar and Microquasar Series - Microquasars in our Galaxy
Quasar and Microquasar Series - Microquasars in our GalaxySérgio Sacani
 
A galactic microquasar mimicking winged radio galaxies
A galactic microquasar mimicking winged radio galaxiesA galactic microquasar mimicking winged radio galaxies
A galactic microquasar mimicking winged radio galaxiesSérgio Sacani
 
The Search Of Nine Planet, Pluto (Artigo Histórico)
The Search Of Nine Planet, Pluto (Artigo Histórico)The Search Of Nine Planet, Pluto (Artigo Histórico)
The Search Of Nine Planet, Pluto (Artigo Histórico)Sérgio Sacani
 
Planeta 9 - A Pan-STARRS1 Search for Planet Nine
Planeta 9 - A Pan-STARRS1 Search for Planet NinePlaneta 9 - A Pan-STARRS1 Search for Planet Nine
Planeta 9 - A Pan-STARRS1 Search for Planet NineSérgio Sacani
 
IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1
IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1
IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1Sérgio Sacani
 
A seven-Earth-radius helium-burning star inside a 20.5-min detached binary
A seven-Earth-radius helium-burning star inside a 20.5-min detached binaryA seven-Earth-radius helium-burning star inside a 20.5-min detached binary
A seven-Earth-radius helium-burning star inside a 20.5-min detached binarySérgio Sacani
 
A review of volcanic electrification of the atmosphere and volcanic lightning
A review of volcanic electrification of the atmosphere and volcanic lightningA review of volcanic electrification of the atmosphere and volcanic lightning
A review of volcanic electrification of the atmosphere and volcanic lightningSérgio Sacani
 
Geological evidence of extensive N-fixation by volcanic lightning during very...
Geological evidence of extensive N-fixation by volcanic lightning during very...Geological evidence of extensive N-fixation by volcanic lightning during very...
Geological evidence of extensive N-fixation by volcanic lightning during very...Sérgio Sacani
 
A recently formed ocean inside Saturn’s moon Mimas
A recently formed ocean inside Saturn’s moon MimasA recently formed ocean inside Saturn’s moon Mimas
A recently formed ocean inside Saturn’s moon MimasSérgio Sacani
 
The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...
The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...
The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...Sérgio Sacani
 
Life, the Universe, andSETI in a Nutshell
Life, the Universe, andSETI in a NutshellLife, the Universe, andSETI in a Nutshell
Life, the Universe, andSETI in a NutshellSérgio Sacani
 
"Space Shuttle: '. . .When data flows, crew and craft are knit into action. ....
"Space Shuttle: '. . .When data flows, crew and craft are knit into action. ...."Space Shuttle: '. . .When data flows, crew and craft are knit into action. ....
"Space Shuttle: '. . .When data flows, crew and craft are knit into action. ....Sérgio Sacani
 

Mehr von Sérgio Sacani (20)

Thermonuclear explosions on neutron stars reveal the speed of their jets
Thermonuclear explosions on neutron stars reveal the speed of their jetsThermonuclear explosions on neutron stars reveal the speed of their jets
Thermonuclear explosions on neutron stars reveal the speed of their jets
 
Identification of Superclusters and Their Properties in the Sloan Digital Sky...
Identification of Superclusters and Their Properties in the Sloan Digital Sky...Identification of Superclusters and Their Properties in the Sloan Digital Sky...
Identification of Superclusters and Their Properties in the Sloan Digital Sky...
 
Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...
Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...
Digitized Continuous Magnetic Recordings for the August/September 1859 Storms...
 
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky Way
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky WayShiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky Way
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky Way
 
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...
 
Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...
Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...
Introducing the Exoplanet Escape Factor and the Fishbowl Worlds (Two conceptu...
 
Revelando Marte - Livro Sobre a Exploração do Planeta Vermelho
Revelando Marte - Livro Sobre a Exploração do Planeta VermelhoRevelando Marte - Livro Sobre a Exploração do Planeta Vermelho
Revelando Marte - Livro Sobre a Exploração do Planeta Vermelho
 
Weak-lensing detection of intracluster filaments in the Coma cluster
Weak-lensing detection of intracluster filaments in the Coma clusterWeak-lensing detection of intracluster filaments in the Coma cluster
Weak-lensing detection of intracluster filaments in the Coma cluster
 
Quasar and Microquasar Series - Microquasars in our Galaxy
Quasar and Microquasar Series - Microquasars in our GalaxyQuasar and Microquasar Series - Microquasars in our Galaxy
Quasar and Microquasar Series - Microquasars in our Galaxy
 
A galactic microquasar mimicking winged radio galaxies
A galactic microquasar mimicking winged radio galaxiesA galactic microquasar mimicking winged radio galaxies
A galactic microquasar mimicking winged radio galaxies
 
The Search Of Nine Planet, Pluto (Artigo Histórico)
The Search Of Nine Planet, Pluto (Artigo Histórico)The Search Of Nine Planet, Pluto (Artigo Histórico)
The Search Of Nine Planet, Pluto (Artigo Histórico)
 
Planeta 9 - A Pan-STARRS1 Search for Planet Nine
Planeta 9 - A Pan-STARRS1 Search for Planet NinePlaneta 9 - A Pan-STARRS1 Search for Planet Nine
Planeta 9 - A Pan-STARRS1 Search for Planet Nine
 
IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1
IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1
IM-1 Press Kit - Kit de Imprensa do Lançmento da Missão IM-1
 
A seven-Earth-radius helium-burning star inside a 20.5-min detached binary
A seven-Earth-radius helium-burning star inside a 20.5-min detached binaryA seven-Earth-radius helium-burning star inside a 20.5-min detached binary
A seven-Earth-radius helium-burning star inside a 20.5-min detached binary
 
A review of volcanic electrification of the atmosphere and volcanic lightning
A review of volcanic electrification of the atmosphere and volcanic lightningA review of volcanic electrification of the atmosphere and volcanic lightning
A review of volcanic electrification of the atmosphere and volcanic lightning
 
Geological evidence of extensive N-fixation by volcanic lightning during very...
Geological evidence of extensive N-fixation by volcanic lightning during very...Geological evidence of extensive N-fixation by volcanic lightning during very...
Geological evidence of extensive N-fixation by volcanic lightning during very...
 
A recently formed ocean inside Saturn’s moon Mimas
A recently formed ocean inside Saturn’s moon MimasA recently formed ocean inside Saturn’s moon Mimas
A recently formed ocean inside Saturn’s moon Mimas
 
The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...
The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...
The BINGO Project IX. Search for fast radio bursts – A forecast for the BINGO...
 
Life, the Universe, andSETI in a Nutshell
Life, the Universe, andSETI in a NutshellLife, the Universe, andSETI in a Nutshell
Life, the Universe, andSETI in a Nutshell
 
"Space Shuttle: '. . .When data flows, crew and craft are knit into action. ....
"Space Shuttle: '. . .When data flows, crew and craft are knit into action. ...."Space Shuttle: '. . .When data flows, crew and craft are knit into action. ....
"Space Shuttle: '. . .When data flows, crew and craft are knit into action. ....
 

Kürzlich hochgeladen

Cloud Revolution: Exploring the New Wave of Serverless Spatial Data
Cloud Revolution: Exploring the New Wave of Serverless Spatial DataCloud Revolution: Exploring the New Wave of Serverless Spatial Data
Cloud Revolution: Exploring the New Wave of Serverless Spatial DataSafe Software
 
Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...
Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...
Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...Will Schroeder
 
Salesforce Miami User Group Event - 1st Quarter 2024
Salesforce Miami User Group Event - 1st Quarter 2024Salesforce Miami User Group Event - 1st Quarter 2024
Salesforce Miami User Group Event - 1st Quarter 2024SkyPlanner
 
How to Effectively Monitor SD-WAN and SASE Environments with ThousandEyes
How to Effectively Monitor SD-WAN and SASE Environments with ThousandEyesHow to Effectively Monitor SD-WAN and SASE Environments with ThousandEyes
How to Effectively Monitor SD-WAN and SASE Environments with ThousandEyesThousandEyes
 
IaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdf
IaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdfIaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdf
IaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdfDaniel Santiago Silva Capera
 
Designing A Time bound resource download URL
Designing A Time bound resource download URLDesigning A Time bound resource download URL
Designing A Time bound resource download URLRuncy Oommen
 
Videogame localization & technology_ how to enhance the power of translation.pdf
Videogame localization & technology_ how to enhance the power of translation.pdfVideogame localization & technology_ how to enhance the power of translation.pdf
Videogame localization & technology_ how to enhance the power of translation.pdfinfogdgmi
 
Using IESVE for Loads, Sizing and Heat Pump Modeling to Achieve Decarbonization
Using IESVE for Loads, Sizing and Heat Pump Modeling to Achieve DecarbonizationUsing IESVE for Loads, Sizing and Heat Pump Modeling to Achieve Decarbonization
Using IESVE for Loads, Sizing and Heat Pump Modeling to Achieve DecarbonizationIES VE
 
UiPath Studio Web workshop series - Day 8
UiPath Studio Web workshop series - Day 8UiPath Studio Web workshop series - Day 8
UiPath Studio Web workshop series - Day 8DianaGray10
 
AI Fame Rush Review – Virtual Influencer Creation In Just Minutes
AI Fame Rush Review – Virtual Influencer Creation In Just MinutesAI Fame Rush Review – Virtual Influencer Creation In Just Minutes
AI Fame Rush Review – Virtual Influencer Creation In Just MinutesMd Hossain Ali
 
UiPath Studio Web workshop series - Day 6
UiPath Studio Web workshop series - Day 6UiPath Studio Web workshop series - Day 6
UiPath Studio Web workshop series - Day 6DianaGray10
 
Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...
Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...
Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...DianaGray10
 
Spring24-Release Overview - Wellingtion User Group-1.pdf
Spring24-Release Overview - Wellingtion User Group-1.pdfSpring24-Release Overview - Wellingtion User Group-1.pdf
Spring24-Release Overview - Wellingtion User Group-1.pdfAnna Loughnan Colquhoun
 
PicPay - GenAI Finance Assistant - ChatGPT for Customer Service
PicPay - GenAI Finance Assistant - ChatGPT for Customer ServicePicPay - GenAI Finance Assistant - ChatGPT for Customer Service
PicPay - GenAI Finance Assistant - ChatGPT for Customer ServiceRenan Moreira de Oliveira
 
COMPUTER 10 Lesson 8 - Building a Website
COMPUTER 10 Lesson 8 - Building a WebsiteCOMPUTER 10 Lesson 8 - Building a Website
COMPUTER 10 Lesson 8 - Building a Websitedgelyza
 
UiPath Studio Web workshop series - Day 7
UiPath Studio Web workshop series - Day 7UiPath Studio Web workshop series - Day 7
UiPath Studio Web workshop series - Day 7DianaGray10
 
Cybersecurity Workshop #1.pptx
Cybersecurity Workshop #1.pptxCybersecurity Workshop #1.pptx
Cybersecurity Workshop #1.pptxGDSC PJATK
 
20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf
20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf
20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdfJamie (Taka) Wang
 
Digital magic. A small project for controlling smart light bulbs.
Digital magic. A small project for controlling smart light bulbs.Digital magic. A small project for controlling smart light bulbs.
Digital magic. A small project for controlling smart light bulbs.francesco barbera
 
Linked Data in Production: Moving Beyond Ontologies
Linked Data in Production: Moving Beyond OntologiesLinked Data in Production: Moving Beyond Ontologies
Linked Data in Production: Moving Beyond OntologiesDavid Newbury
 

Kürzlich hochgeladen (20)

Cloud Revolution: Exploring the New Wave of Serverless Spatial Data
Cloud Revolution: Exploring the New Wave of Serverless Spatial DataCloud Revolution: Exploring the New Wave of Serverless Spatial Data
Cloud Revolution: Exploring the New Wave of Serverless Spatial Data
 
Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...
Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...
Apres-Cyber - The Data Dilemma: Bridging Offensive Operations and Machine Lea...
 
Salesforce Miami User Group Event - 1st Quarter 2024
Salesforce Miami User Group Event - 1st Quarter 2024Salesforce Miami User Group Event - 1st Quarter 2024
Salesforce Miami User Group Event - 1st Quarter 2024
 
How to Effectively Monitor SD-WAN and SASE Environments with ThousandEyes
How to Effectively Monitor SD-WAN and SASE Environments with ThousandEyesHow to Effectively Monitor SD-WAN and SASE Environments with ThousandEyes
How to Effectively Monitor SD-WAN and SASE Environments with ThousandEyes
 
IaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdf
IaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdfIaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdf
IaC & GitOps in a Nutshell - a FridayInANuthshell Episode.pdf
 
Designing A Time bound resource download URL
Designing A Time bound resource download URLDesigning A Time bound resource download URL
Designing A Time bound resource download URL
 
Videogame localization & technology_ how to enhance the power of translation.pdf
Videogame localization & technology_ how to enhance the power of translation.pdfVideogame localization & technology_ how to enhance the power of translation.pdf
Videogame localization & technology_ how to enhance the power of translation.pdf
 
Using IESVE for Loads, Sizing and Heat Pump Modeling to Achieve Decarbonization
Using IESVE for Loads, Sizing and Heat Pump Modeling to Achieve DecarbonizationUsing IESVE for Loads, Sizing and Heat Pump Modeling to Achieve Decarbonization
Using IESVE for Loads, Sizing and Heat Pump Modeling to Achieve Decarbonization
 
UiPath Studio Web workshop series - Day 8
UiPath Studio Web workshop series - Day 8UiPath Studio Web workshop series - Day 8
UiPath Studio Web workshop series - Day 8
 
AI Fame Rush Review – Virtual Influencer Creation In Just Minutes
AI Fame Rush Review – Virtual Influencer Creation In Just MinutesAI Fame Rush Review – Virtual Influencer Creation In Just Minutes
AI Fame Rush Review – Virtual Influencer Creation In Just Minutes
 
UiPath Studio Web workshop series - Day 6
UiPath Studio Web workshop series - Day 6UiPath Studio Web workshop series - Day 6
UiPath Studio Web workshop series - Day 6
 
Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...
Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...
Connector Corner: Extending LLM automation use cases with UiPath GenAI connec...
 
Spring24-Release Overview - Wellingtion User Group-1.pdf
Spring24-Release Overview - Wellingtion User Group-1.pdfSpring24-Release Overview - Wellingtion User Group-1.pdf
Spring24-Release Overview - Wellingtion User Group-1.pdf
 
PicPay - GenAI Finance Assistant - ChatGPT for Customer Service
PicPay - GenAI Finance Assistant - ChatGPT for Customer ServicePicPay - GenAI Finance Assistant - ChatGPT for Customer Service
PicPay - GenAI Finance Assistant - ChatGPT for Customer Service
 
COMPUTER 10 Lesson 8 - Building a Website
COMPUTER 10 Lesson 8 - Building a WebsiteCOMPUTER 10 Lesson 8 - Building a Website
COMPUTER 10 Lesson 8 - Building a Website
 
UiPath Studio Web workshop series - Day 7
UiPath Studio Web workshop series - Day 7UiPath Studio Web workshop series - Day 7
UiPath Studio Web workshop series - Day 7
 
Cybersecurity Workshop #1.pptx
Cybersecurity Workshop #1.pptxCybersecurity Workshop #1.pptx
Cybersecurity Workshop #1.pptx
 
20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf
20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf
20200723_insight_release_plan_v6.pdf20200723_insight_release_plan_v6.pdf
 
Digital magic. A small project for controlling smart light bulbs.
Digital magic. A small project for controlling smart light bulbs.Digital magic. A small project for controlling smart light bulbs.
Digital magic. A small project for controlling smart light bulbs.
 
Linked Data in Production: Moving Beyond Ontologies
Linked Data in Production: Moving Beyond OntologiesLinked Data in Production: Moving Beyond Ontologies
Linked Data in Production: Moving Beyond Ontologies
 

Investigating the nuclear_activity_of_ngc1672

  • 1. D RAFT VERSION A PRIL 12, 2011 Preprint typeset using LTEX style emulateapj v. 11/10/09 A INVESTIGATING THE NUCLEAR ACTIVITY OF BARRED SPIRAL GALAXIES: THE CASE OF NGC 1672 L. P. J ENKINS 1,2 , W. N. B RANDT 3,4 , E. J. M. C OLBERT 2 , B. KORIBALSKI 5 , K. D. K UNTZ 2 , A. J. L EVAN 6 , R. O JHA 7 , T. P. ROBERTS 8 , M. J. WARD 8 , A. Z EZAS 9 Draft version April 12, 2011 ABSTRACT We have performed an X-ray study of the nearby barred spiral galaxy NGC 1672, primarily to ascertain the arXiv:1104.1649v1 [astro-ph.CO] 8 Apr 2011 effect of the bar on its nuclear activity. We use both Chandra and XMM-Newton observations to investigate its X-ray properties, together with supporting high-resolution optical imaging data from the Hubble Space Telescope (HST), infrared imaging from the Spitzer Space Telescope, and ATCA ground-based radio data. We detect 28 X-ray sources within the D25 area of the galaxy, many of which correlate spatially with star- formation in the bar and spiral arms, while two are identified as background galaxies in the HST images. Nine of the X-ray sources are ULXs, with the three brightest (LX > 5 × 1039 erg s−1 ) located at the ends of the bar. With the spatial resolution of Chandra, we are able to show for the first time that NGC 1672 possesses a hard (Γ ∼ 1.5) nuclear X-ray source with a 2–10 keV luminosity of 4 × 1038 erg s−1 . This is surrounded by an X-ray bright circumnuclear star-forming ring, comprised of point sources and hot gas, which dominates the 2–10 keV emission in the central region of the galaxy. The spatially resolved multiwavelength photometry indicates that the nuclear source is a low-luminosity AGN (LLAGN), but with star formation activity close to the central black hole. A high-resolution multiwavelength survey is required to fully assess the impact of both large-scale bars and smaller-scale phenomena such as nuclear bars, rings and nuclear spirals on the fueling of LLAGN. Subject headings: galaxies: individual (NGC 1672) – galaxies: nuclei – galaxies: spiral – galaxies: evolution 1. INTRODUCTION material is also believed to build ‘pseudobulges’, which are The presence of a bar in a galaxy plays an impor- distinct from classical galaxy bulges (Kormendy & Kennicutt tant role in its evolution. Approximately two-thirds of 2004). A strong global density pattern such as a bar can also all spiral galaxies are barred (e.g. Eskridge et al. 2000; produce a series of resonances between the angular velocity Men´ ndez-Delmestre et al. 2007), so any complete picture of e of the bar and the orbital motions of stars and gas in the disk, galaxies must include the impact of bars on both their nu- where rings can form (Buta 1999). Indeed, some galaxies clear and extra-nuclear properties. Secular (i.e. internal) with bars are known to have circumnuclear rings of star for- galaxy evolution involving bars, oval distortions and spiral mation (e.g. Buta & Combes 1996; Knapen 2005a), resulting structure can have a significant effect when a galaxy is no from increased gas density at or near the Inner Lindblad Res- longer merging or interacting strongly with other galaxies (see onance (ILR). Kormendy & Kennicutt 2004). For example, there is believed A question that we are addressing with this study is, can the to be a causal connection between the existence of a bar and material driven to the center of a galaxy by the bar also fuel a galaxy’s circumnuclear properties. Bars can drive gas from an active galactic nucleus (AGN)? While there is clear obser- the outer disk to the inner regions of the galaxy; gas clouds vational evidence that bars in disk galaxies cause higher cen- are shocked as they encounter the leading edge of the bar, tral concentrations of gas (and hence centrally concentrated lose angular momentum, and flow towards the galaxy’s center star formation) compared to non-barred galaxies, it is unclear (Shlosman et al. 1990). An observable result of this is that a whether a large-scale bar is sufficient to transport material substantial fraction of galaxies with bars show enhanced star- close enough for AGN feeding (typically on AU scales, see formation activity in their central regions, and the inflow of Knapen 2005b for a review). Additionally, in an X-ray study by Maiolino et al. (1999) using Ginga, ASCA and BeppoSAX data, a strong correlation was found between absorbing col- 1 Laboratory for X-ray Astrophysics, NASA Goddard Space Flight Cen- umn density toward Type-2 Seyfert nuclei and the presence ter, Code 662, Greenbelt, MD 20771, USA of a strong bar, i.e. more than 80% of Compton-thick Seyfert 2 Johns Hopkins University, 3400 N. Charles St, Baltimore, MD 21218, USA 2s are barred. This suggests that if a low-luminosity AGN 3 Department of Astronomy & Astrophysics, The Pennsylvania State (LLAGN) is present, it may be obscured from view at optical University, 525 Davey Lab, University Park, PA 16802, USA wavelengths and/or diluted by strong star-formation activity, 4 Institute for Gravitation and the Cosmos, The Pennsylvania State Uni- which could lead to a misclassification as a pure star-forming versity, University Park, PA 16802, USA 5 CSIRO, Australia Telescope National Facility (ATNF), PO Box 76, nucleus. Epping NSW 1710, AUSTRALIA The topic of the influence of bars on galaxy evolution is 6 Department of Physics, University of Warwick, Coventry, CV4 7AL, not well studied at X-ray energies, but we are now able UK to utilize the excellent complementary imaging and spec- 7 NVI/United States Naval Observatory, 3450 Massachusetts Ave NW, tral capabilities of Chandra and XMM-Newton to make de- Washington DC 20392, USA 8 Department of Physics, Durham University, South Road, Durham, tailed investigations of the X-ray characteristics of these sys- DH1 3LE, UK tems. In particular, high-spatial-resolution X-ray observa- 9 Department of Physics, University of Crete, PO Box 2208, GR-71003 tions with Chandra provide an ideal method for search- Heraklion, Greece ing for low-level AGN activity in nearby galaxies, in the
  • 2. 2 Jenkins et al. form of a hard central point source that may not be vis- ring of star formation, measuring ∼ 11′′ × 9′′ (0.9 × 0.7 kpc ible at other wavelengths. It also allows us to separate at a distance of 16.3 Mpc), located between two ILRs. There- potential AGN activity from other types of X-ray sources fore, studies of its nuclear properties that use large apertures that may reside close to the nucleus, such as X-ray bina- are strongly affected by the star-formation in the ring. For ries (XRBs) associated with circumnuclear star-formation. example, Osmer et al. (1974) showed that the optical emis- Indeed, X-ray surveys utilizing Chandra have proved suc- sion spectrum in the central 17′′ was similar to those of cessful in recent years in identifying previously unknown normal HII nuclei, but with an Hα/Hβ ratio indicative of LLAGN activity in nearby galaxies. In particular, X-ray nu- a large amount of dust reddening. Storchi-Bergmann et al. clei spanning a wide range of X-ray luminosities (∼ 1037 − (1995) also measured optical emission-line ratios in a rela- 1044 erg s−1 , 2–10 keV) have been detected in a large frac- tively large 10′′ × 20′′ aperture, and classified the nucleus as tion (typically ∼45–70%) of galaxies hosting low-ionization ‘composite’, with ratios between those of typical starburst and nuclear emission regions (LINERs; Heckman 1980), as well Seyfert values. More recent optical line ratio diagnostics by as galaxies classed as having HII or transition nuclei (e.g. Kewley et al. (2000) of the emission within a ∼ 13′′ slit are Ho et al. 2001; Terashima & Wilson 2003; Satyapal et al. indicative of an HII-type nucleus, with no Hα line broadening 2004; Satyapal et al. 2005; Dudik et al. 2005; Flohic et al. detected. All of these studies will have been strongly contam- 2006; Gonz´ lez-Mart´n et al. 2006; Gonz´ lez-Mart´n et al. a ı a ı inated by the emission from the circumnuclear starburst ring; 2009; Zhang et al. 2009; Desroches & Ho 2009). Studies at however they do demonstrate that this component is domi- other wavelengths have also recently been used to uncover nant, and that any potential AGN activity would be relatively previously unknown AGN activity in nearby galaxies. For weak. example, Spitzer infrared (IR) spectroscopic surveys have re- More detailed, spatially resolved studies have also given vealed bonafide AGN in both LINERs and IR-bright galax- ambiguous results. Veron et al. (1981) detected possible ies, some of which showed no sign of such activity in opti- broadening of [O III] (∼300 km s−1 ) compared to Hβ lines cal studies (Dudik et al. 2009; Goulding & Alexander 2009). (∼150 km s−1 ) in the central 2′′ × 4′′ , which they sug- High-resolution radio imaging has been shown to be an effi- gested was evidence of a composite HII/Seyfert 2 nu- cient method for finding LLAGN activity; compact radio nu- cleus. Garcia-Vargas et al. (1990) performed a high-spatial- clei have been found in 50% of LINERs/LLAGN, which are resolution spectral analysis of the nucleus, and found a strong thought to be attributable to relativistic jets produced by ac- increase in the [O III]/Hβ ratio in the central 1′′ compared creting super-massive black holes (Nagar et al. 2005 and ref- to its immediate surroundings. However, both lines had the erences therein). same FWHM of ∼300 km s−1 , and the authors classified To begin to address the nature of the nuclear (and off- the nucleus as a LINER. Storchi-Bergmann et al. (1996) also nuclear) X-ray emission in barred galaxies, we have con- measured spatially-resolved (2′′ ) emission-line ratios, which ducted a pilot study of the barred galaxy NGC 1672, using were better modeled by a LINER-type stellar photoionization X-ray observations from both Chandra (40 ks) and XMM- model with Tef f ≥ 45, 000 K, rather than photoionization by Newton (50 ks). Here we report the results from these ob- a strong AGN continuum. servations, and use supporting HST/ACS, Spitzer and ATCA NGC 1672 has previously been observed with at X-ray radio observations to assist in the interpretation of the X-ray wavelengths with ROSAT and ASCA. Three bright X-ray results. This paper is laid out as follows. In § 2 we give back- sources were detected in the soft 0.2–2.0 keV band with the ground information on the target galaxy NGC 1672. In § 3, we ROSAT HRI and PSPC, which were clearly associated with describe the Chandra, XMM-Newton, HST/ACS, Spitzer and the galaxy (Brandt et al. 1996; de Naray et al. 2000). The ATCA radio observations and data analysis techniques, and brightest source was located at the nucleus, and the other two in § 4 we present our results. In § 5 we discuss the nature of were cospatial with the ends of the bar. The nucleus had a the nuclear emission, and in § 6 we compare our results with soft X-ray spectrum consistent with thermal emission with those for other barred and non-barred galaxies in the litera- a temperature of 0.68 keV, with a soft X-ray luminosity of ture. Throughout this paper we use a distance to NGC 1672 7 × 1039 erg s−1 (0.2–2.0 keV). However, these studies were of 16.3 Mpc, corresponding to a recession velocity of 1140 km again unable to resolve the nuclear emission spatially due to s−1 relative to the centroid of the Local Group (Osmer et al. the 5′′ FWHM of the HRI point-spread-function (PSF), and 1974), with H0 =70 km s−1 Mpc−1 . so could not determine whether the bulk of the soft emission came from a starburst or AGN. Furthermore, the ASCA data 2. NGC 1672 showed no evidence of significant hard (2–10 keV) emission For this pilot study, we have selected the nearby (16.3 Mpc) from the nuclear source, with the hard emission in the galaxy late-type barred spiral galaxy NGC 1672 (SB(r)bc). It being dominated by two off-nuclear X-ray sources (X-3 and has a moderately low inclination angle (i = 34◦ , X-7, see figure 4b in de Naray et al. 2000). Thus, it was con- de Vaucouleurs et al. 1991), and is known to have a strong cluded that if an active nucleus is present in NGC 1672, it bar (2.4′ in length, corresponding to 11.4 kpc at a distance must be Compton-thick, with NH > 2 × 1024 cm−2 . of 16.3 Mpc), many HII regions in its four spiral arms, plus vigorous star formation at the ends of the bar (Brandt et al. 1996, and references therein). It has a high IR luminosity (log 3. OBSERVATIONS AND DATA REDUCTION LF IR /L⊙ = 10.2), and a global star formation rate (SFR) of 2.7 M⊙ yr−1 (Kewley et al. 2000). 3.1. Chandra Observations Optical studies have given conflicting evidence as to the NGC 1672 was observed with Chandra for 40 ks on April nature of the nuclear activity in NGC 1672. It was noted 30, 2006 (ObsID 5932) using the back-illuminated S3 chip by S´ rsic & Pastoriza (1965) as having a complex or ‘amor- e of the Advanced CCD Imaging Spectrometer (ACIS). The phous’ nuclear morphology, and was subsequently shown by field of view of the observation is shown in Figure 1; the Storchi-Bergmann et al. (1996) to possess a circumnuclear nucleus of the galaxy was placed at the aimpoint of the S3
  • 3. Investigating the nuclear activity of barred spiral galaxies 3 1’ Figure 1.DSS optical image of NGC1672 showing the Chandra ACIS-S field of view (solid red), the HST/ACS field of view (dotted blue), and the 3- and 6-cm radio beam sizes (dashed green circles of 5.5′ and 9.8′ diameters respectively). The D25 ellipse of the galaxy is shown with a solid (black) line. The XMM-Newton and Spitzer observations cover the D25 area of the galaxy. North is up, east to the left. chip, and the observation encompasses the entire D25 10 ex- Initial detection of candidate sources was carried out in tent of the galaxy. The data were initially processed with the each energy-band image using the CIAO task wavdetect, Chandra Interactive Analysis of Observations (CIAO) tool a Mexican Hat wavelet source detection algorithm. Wavelet suite version 3.3, with CALDB version 3.2.1. The process- scales of 1.0, 1.414, 2.0, 2.828, 4.0, 5.657 & 8.0 pixels were ing included a charge transfer efficiency (CTI) correction and used, and the significance threshold was set to 1.0 × 10−6 time-dependent gain correction. Further data analysis was corresponding to approximately one false detection per band performed using CIAO version 3.4. A full-field light curve over the 8×8′ field. A merged source list was created that in- was extracted from the level-2 event list to search for periods cluded sources detected in all bands, which was used as the in- of high background, but no strong flares were found, leaving put list for source parameterization in the ACIS Extract12 a net exposure time of 39.6 ks. IDL software (AE; Broos et al. 2010). The main steps in the procedure are (1) the definition of source extraction regions 3.1.1. Imaging & Source Detection based on the 90% contour of the local PSF, (2) trial extrac- tion of events within those regions, (3) improvement of po- The basic data reduction was done using standard CIAO sitions if necessary (see below), (4) full extraction of source data analysis threads.11 Images were created of an 8′ ×8′ and background spectra using final positions, and the creation region (encompassing the full D25 area of the galaxy) at of associated RMFs and ARFs for each source. full 0.492′′ pixel resolution in soft (0.3–1 keV), medium Source positions were improved (in step 3) using the (1–2 keV), hard (2–10 keV) and broad (0.3–10 keV) energy CHECK POSITIONS stage, which computes “mean data” bands. Monochromatic exposure maps were created at 0.8, and “correlation” positions for all sources. The “mean data” 1.0 and 2.0 keV, corresponding to the peak energy in the soft, position corresponds to the central position of the extracted in- medium and hard band data. The images were adaptively band events in the 0.3–10 keV band, while the “correlation” smoothed using the csmooth task, with a fairly low sig- positions are obtained by convolving the data image with a nificance of 2σ above the local background (corresponding position-dependent model PSF. The offsets between these and to ∼1–30 pixels in the body of the galaxy) to avoid over- the original wavdetect positions were typically 0.1–0.8′′. smoothing of faint features in the central region (see § 4.3). The position estimates were visually reviewed, and the best 10 D was chosen for each source. Where there was little difference 25 = the apparent major isophotal diameter measured at the surface brightness level µB = 25.0 mag/arcsec2 11 http://asc.harvard.edu/ciao/threads/index.html 12 http://www.astro.psu.edu/xray/docs/TARA/ae users guide.html
  • 4. 4 Jenkins et al. between the estimates, the original position was retained. data (images and spectra) were created using standard pat- The source extraction regions were based on the 90% con- terns corresponding to single and double pixel events for the tour of the local PSF at the final positions. Background spec- PN (0–4), and patterns 0–12 (single to quadruple events) for tra were extracted in local annuli, with inner radii of 1.1 times the MOS cameras. For spectral extraction, the quality flag of the 99% radius of the PSF (to exclude any residual source was set to zero to reject events from bad pixels and events too flux), and outer radii tailored so that each background spec- close to the CCD chip edges. trum contains at least 100 counts. For the central (ring) re- gion, the whole area (17′′ radius) was masked out from the 3.2.1. Imaging & Source Detection background map due to the clumpy diffuse emission in the Multi-band source detection was performed on the PN and area, and the background subtraction for sources in this re- MOS data, using the methods detailed in Jenkins et al. (2005). gion (except for the nucleus) was performed using the area In brief, images were created in the following energy bands: immediately outside this. soft (0.3–1 keV), medium (1–2 keV) and hard (2–10 keV). Ex- Due to the complexity of the central region, the spec- posure maps were created for each instrument/energy band trum of the nuclear X-ray source was extracted manually in using the SAS task EEXPMAP, and detector masks were cre- CIAO using specextract. The source aperture was set ated for each camera with EMASK. Two methods of initial to 1.2′′ radius, centered on the position from wavdetect source recognition were used: EBOXDETECT, a sliding-box (04h45m 42.5s , −59◦ 14′ 50.1′′ ). The local background flux algorithm that simultaneously searches the three energy band was measured in an annulus immediately outside this (1.2– images, and EWAVELET, a Mexican hat wavelet detection 2.0′′ radius), and was chosen using the radio contours as a routine that works on individual images. Both used back- guide in order to cover as much of the area inside the ring, ground maps created with ASMOOTH. The source lists from without encountering any ring emission (see § 4.3). Any other both methods were then parameterized using EMLDETECT, typical non-local background region would have left residual which performs maximum likelihood PSF fits to each source. soft emission in the nuclear source counts. These were then compared, and any additional sources de- Since there is significant diffuse emission in the circum- tected with EWAVELET were added to the EBOXDETECT nuclear ring area, it is possible that some of the candidate source list, and the parameterization repeated. All sources sources detected there may be clumpy gas rather than true significant at > 4σ in at least one energy band, and within point sources. To test this, we performed PSF fitting using the the D25 ellipse of NGC 1672, were retained and visually in- AE task AE RADIAL PROFILE, which computes a 1-sided spected. Spectra, ARFs and RMFs were extracted from the KS probability to determine whether the observed counts in data for each source using the SAS task especget. the 1–2 keV energy range are consistent with the model lo- The final XMM-Newton catalog contains 19 extra-nuclear cal 1.49 keV PSF encircled energy distribution. Six candidate sources, and their properties are listed in Table 1 along with sources in the ring region were inconsistent with the local PSF the corresponding Chandra properties. The source fluxes profile with a significance of > 99%. Sources without detec- were again determined using spectral fitting (see § 3.3). Note tions in the hard 2–10 keV band and with a KS probability that six sources (including the nucleus) within the central > 99% were deemed to be diffuse and discarded. ∼20′′ radius are not spatially resolved with XMM-Newton; The final Chandra catalog contains 28 sources inside the these are marked with (N)=nucleus and (C)=central region D25 ellipse, and their properties are listed in Table 1. Sources source. Apart from #10, 17 and 24, all other sources detected with significance of > 2.5σ were retained, including faint in the Chandra observation are detected in the XMM-Newton Chandra counterparts to two significantly detected XMM- observation. Newton sources (for variability and completeness). This detection threshold corresponds to >12 net source counts. 3.3. X-ray Source Spectral Fits Source fluxes were determined using spectral fitting (see § 3.3). To estimate source fluxes reliably, we have performed spec- The absolute astrometry of Chandra is generally accurate tral fitting on each source using XSPEC v12. Detailed spec- to within ∼1′′ . 13 To confirm this, the X-ray positions were tral fitting was performed on Chandra sources with > 100 net compared to the 2MASS point source catalog. Three coun- counts, and on XMM-Newton sources with > 100 net counts terparts were found in the field; the offsets between the X-ray in either the PN or MOS data. These spectra were binned and 2MASS positions were small (0.14, 0.16 & 0.6′′ ), and in (grouped to a minimum of 20 counts per bin) and fitted, using non-uniform directions, with the greatest offset for a source χ2 statistics, with both powerlaw+absorption (PO*WABS) 4′ off-axis at the edge of the field. Given this accuracy, no and disk blackbody+absorption (DISKBB*WABS) models. astrometric correction was made to the Chandra positions. In all cases, the powerlaw model provided the best fit. Spec- tral parameters and corresponding 0.3–10 keV fluxes and lu- 3.2. XMM-Newton Observations minosities are shown in Table 1. For the XMM-Newton data, NGC 1672 was observed with XMM-Newton for 50 ks on the PN, MOS1 and MOS2 spectra were fitted simultaneously. November 27, 2004 (ObsID 0203880101). The EPIC MOS- The fluxes and errors from the three instruments were com- 1, MOS-2 and PN cameras were operated with medium filters bined to provide a weighted mean flux for each source using in Prime Full Window mode. Full-field light curves were ac- the method of Barlow (2004).14 cumulated for the three exposures in the 10–15 keV band to For sources with < 100 net counts, a simple power- check for high background intervals of soft proton flares. The law+Galactic absorption model was fitted to unbinned spec- data were found to be clean for the duration of the observa- tra using the C-statistic (Cash 1979). Since at such low tion, and the full time intervals were used in subsequent anal- count rates source parameters are difficult to constrain, the ysis: 47.9 ks (PN), 49.4 ks (MOS1) & 49.5 ks (MOS2). All powerlaw and absorption parameters were frozen (Γ = 1.7, 13 http://cxc.harvard.edu/cal/ASPECT/celmon/ 14 http://www.slac.stanford.edu/∼barlow/statistics.html
  • 5. Investigating the nuclear activity of barred spiral galaxies 5 NHGal = 0.223 × 1021 cm−2 ), with the normalization as the An alternative to direct PSF subtraction is to use a nar- only free parameter. The resulting fluxes and luminosities are row aperture for the determination of the light within the nu- also shown in Table 1. The source properties are described in cleus, and then to apply the aperture corrections tabulated by § 4.1. Sirianni et al. (2005). We used a 0.1′′ (2 pixel) radius aper- ture, and subtracted the background using an 1.2–2′′ annulus 3.4. Multi-wavelength data centered on the nucleus. To compare directly with the Chan- 3.4.1. HST-ACS Observations dra observations, we have also performed photometry using the same physical aperture (1.2′′ radius) and background an- NGC 1672 was observed by the Hubble Space Telescope nulus (again 1.2–2′′ ). The resulting magnitudes from these (HST) on August 1, 2005 using the Advanced Camera for methods are also shown in Table 2. Surveys (ACS) Wide Field Channel (WFC) in the broad- The upper limits measured using the PSF subtraction band F435W, F550M and F814W filters, plus the narrow-band method are similar to the measurements obtained from the F658N (Hα) filter. A large dither was implemented, covering narrow aperture, though there is a good deal of scatter be- the dimensions of one of the WFC chips in order to fit the vis- tween these and the larger Chandra aperture measurements. ible disk of the galaxy into each observation (see Figure 1). Given that PSF subtraction gives the most stringent con- Exposure times were 2444 s in each observation, split into straints on the magnitude of a nuclear point source, we adopt four separate observations corresponding to the visibility of these limits for the multiwavelength comparison (see Table 3), NGC 1672 in each single orbit. We also include in our analy- and the construction of the nuclear spectral energy distribu- sis an archival ACS High Resolution Channel (HRC) F330W tion (SED, see § 5.2). The AB magnitudes were converted UV observation of the nucleus of NGC 1672, taken July 19, to flux density using ABmag = −2.5 log Fν − 48.6,16 and 2002, with an exposure time of 1140 s. All of the ACS ob- then into luminosity using νLν = 4πd2 Fν ×Central filter fre- servations were processed through the standard multidrizzle quency.17 We note that the centroid of the emission in the pipeline (Koekemoer et al. 2002). As sub-pixel dithers were F330W images does not correspond with that seen in data not used in the observations, the drizzle parameters pixfrac taken at longer wavelengths, which suggests that there is some and scale were set to unity, preserving the native pixel scale of extinction along the line-of-sight. both the HRC and WFC. Each of the ACS WFC images were astrometrically registered with 2MASS stellar objects falling 3.4.2. Spitzer IR Observations within the FOV, yielding an astrometric fit with an RMS of ∼ 0.15′′ . The F658N image is significantly contaminated by NGC 1672 was observed with the Spitzer Infrared Ar- continuum emission within the Hα passband; we therefore ray Camera (IRAC, Fazio et al. 2004) on November 29 2006 created a continuum-subtracted image (denoted F658CS) us- (Program ID 30496, PI Fisher). Basic Calibrated Data (BCD) ing a continuum image estimated from a linear combination of were retrieved from the archive at 3.6, 4.5, 5.8 and 8.0µm. the F550M and F814W images (weighted by their separation We performed post-BCD processing (mosaicing, with a plate from the Hα line, and multiplied by the relative sensitivity of scale of 0.86 arcsec/pixel) using the Spitzer data-processing each filter to obtain the same physical units in each image). package MOPEX (Makovoz et al. 2006). The images are flux The ACS images have a very high spatial resolution of calibrated in the pipeline in units of surface brightness (MJy ∼0.1′′ . They show that, while the optical emission peaks sr−1 ), and we converted them to flux density units by mul- in the central 2′′ nuclear region, it is clearly non-point like tiplying by a conversion factor of 1MJy sr−1 = 17.38 µJy with a FWHM of ∼30 pixels (1.5′′ ). Indeed it displays a per pixel. This is a combination of the conversion given in complex/irregular morphology, and in a visual inspection we the Spitzer Observers Manual (1MJy sr−1 = 23.50443 µJy found no obvious point sources that could correspond to, arcsec−2 ), and the pixel solid angle (0.74 arcsec2 ). A MIPS for example, a nuclear star cluster (which are generally only (multi-band imaging photometer) 24µm calibrated image was “marginally resolved ” in HST images of nearby galaxies, also retrieved from the archive (from the same Spitzer pro- B¨ ker et al. 2004). The complexity and extended nature of o gram), which was reduced using standard pipeline processing. the region suggests that the use of any moderate sized photo- A stellar-continuum subtracted 8.0µm (PAH) image was cre- metric aperture will result in a significant overestimate of the ated to highlight the star-forming regions, using a conversion true flux from the nucleus. We investigated this in three ways: based on a standard model of the starlight near-IR SED; this (1) via PSF subtraction, (2) narrow aperture photometry, and is 8.0µm − 0.232×3.6µm (Helou et al. 2004). (3) photometry using the Chandra aperture. Photometry was performed on the nuclear source in the four ′′ To estimate the maximum magnitude of any point source at IRAC bands using a 1. 5 radius aperture centred on the Chan- the center of the galaxy, PSFs were constructed from isolated dra position of the nucleus, using a local annular background point sources in each image and subtracted from the centroid between 2.5–3.0′′. This aperture was chosen because of the of the galaxy light in each band, scaled such that their cores larger PSF of IRAC (1.4–1.7′′ FWHM, Fazio et al. 2004), and resulted in a roughly zero flux value for the brightest pixel aperture corrections were applied as detailed in the IRAC in the galaxy core. For two filters it was not possible to ob- Data Handbook v3.0, section 5.5.1. The resulting flux den- tain actual PSFs from the images. In the case of F330W, the sities (and AB magnitudes) are shown in Table 3. Note that HRC field of view is too small for any bright, isolated sources photometry is not performed on the MIPS data, as the spatial to be present, while in our F658N continuum-subtracted im- resolution (∼6′′ ) is insufficient to separate the nuclear source age the stars were largely subtracted. To overcome this, we from the circumnuclear ring emission. used TinyTim15 to create artificial PSFs for these filters, which were then subtracted from the data. The resulting upper limits 3.4.3. Radio Observations are shown in Table 2. 16 http://www.stsci.edu/hst/acs/analysis/zeropoints 15 http://www.stecf.org/instruments/TinyTim/ 17 http://acs.pha.jhu.edu/instrument/filters/general/Master Table.html
  • 6. 6 Jenkins et al. Chandra XMM 1’ (a) 1’ (b) Spitzer Chandra (diffuse) 1’ (c) 1’ (d) Figure 2. (a) Chandra 3-color ACIS-S image of NGC 1672: red = 0.3–1 keV, green = 1–2 keV, blue = 2–10 keV. (b) XMM-Newton EPIC (MOS1+MOS2+PN) 3-color image (in the same energy bands). (c) Spitzer 3-color image: red = 24µm (MIPS), green = 8µm (IRAC), blue = 3.6µm (IRAC). (d) Chandra 3-color image of the diffuse X-ray emission. Contours from the Spitzer IRAC stellar-continuum-subtracted 8µm data are overlaid, which are spatially correlated with the X-ray emission. The D25 ellipse of the galaxy is shown with a dashed white line. All images are on the same scale and co-aligned. North is up, east to the left. Radio continuum observations of NGC 1672 were ob- at 4800 MHz and 4928 MHz, with bandwidths of 128 MHz tained at 3-cm and 6-cm with the Australia Telescope Com- divided into 32 channels. At 4864 MHz the ATCA primary pact Array (ATCA). Data reduction was carried out with the beam is 9.8′ . The data from both frequency bands were com- MIRIAD 18 software package, using standard procedures. bined, resulting in an angular resolution of 1.9′′ ×1.7′′ and an The 3-cm image was created using archival data from a rms of 0.04 mJy/beam. The source PKS B1934–638 was used 1.5C configuration obtained in May 2003 and a 6D configura- as the primary (amplitude & bandpass) calibrator, and PKS tion obtained in July 2003, with on-source integration times B0522–611 and PKS B0420–625 were used as the secondary of 9 h and 10 h respectively. Both observations consist of (phase) calibrators at 3- and 6-cm, respectively. two frequency bands centered at 8640 MHz and 8768 MHz, A point source fit to the nuclear source gives a position with bandwidths of 128 MHz divided into 32 channels. At of α, δ(J2000) = 04h 45m 42.50s, −59◦ 14′ 49.85′′ (±0.12′′). 8700 MHz the ATCA primary beam is 5.5′ . The data for We measure peak fluxes of 0.95 ± 0.15 mJy at 3-cm and both observations/frequency bands were combined using ‘ro- 1.62±0.15 mJy at 6-cm. We measure integrated flux densities bust’ weighting (r = 0), resulting in an angular resolution of 34 mJy (3-cm) and 35 mJy (6-cm) for the radio continuum of 1.3′′ ×1.0′′ and an rms of 0.03 mJy/beam. The 6-cm im- emission from both the nuclear source and surrounding star- age was created using archival data in the 6A configuration forming ring. It is likely that some extended flux has been obtained in May 2002, with an on-source integration time of resolved out by the interferometer. Single-dish radio contin- 11 h. The observation consists of two frequency bands centred uum flux estimates of NGC 1672 (PMN J0445–5914, PKS J0445–5915) at ∼5 GHz (6-cm) are typically around 100 mJy 18 http://www.atnf.csiro.au/computing/software/miriad/ (see Wright et al. 1994; Harnett 1987).
  • 7. Investigating the nuclear activity of barred spiral galaxies 7 Figure 3.HST/ACS 3-color image of NGC 1672, produced by Zolt Levay at the Space Telescope Science Institute. The colors correspond to: red=combined F658N (Hα) + F814W (I), green = F550M (V ), blue = F435W (B). The image is 4.4′ × 3.2′ in size, with an orientation such that north is 34◦ east (left) of the y-axis. There is also one other radio source in the field of view at detected within the D25 area of the galaxy (blue crosses). α, δ(J2000) = 04h 45m 36.70s, −59◦ 14′ 28.00′′ (±0.03′′), with Note that we do not plot the source positions on the HST im- flux densities of 1.5 ± 0.1 mJy (3-cm) and 1.4 ± 0.1 mJy (6- age here since it does not cover the entire D25 area. The po- cm). This is positionally coincident with X-ray source #8 sitions correlate well with the optical structure of the galaxy, (044536.73–591428.0). with sources concentrated in the nuclear region (see § 4.3) and spread throughout the disk and spiral arms. The extra-nuclear 4. RESULTS source fluxes range between FX = 2.3 × 10−15 − 2.8 × 10−13 Figure 2(a–c) shows 3-color Chandra, XMM-Newton and erg s−1 cm−2 over both XMM-Newton and Chandra observa- Spitzer IRAC images of the entire D25 area of NGC 1672. tions, corresponding to LX = 7.4 × 1037 − 9.0 × 1039 erg The X-ray sources outside the nuclear region are well re- s−1 at the distance of NGC 1672. solved in both the Chandra and XMM-Newton data, and are Nine sources, almost a third of the population, reach ul- discussed in § 4.1. There is also a diffuse hot X-ray gas com- traluminous X-ray source (ULX) luminosities (LX > 1039 ponent, which is shown in Figure 2(d) as extended red/green erg s−1 , 0.3–10 keV) in either one or both X-ray observa- X-ray emission (see § 4.2). The nuclear region is very bright tions; these are marked with red circles (sources 1, 4, 5, 6, at all wavelengths, and will be discussed in detail in § 4.3. 7, 13, 24, 25 and 28). Three of the ULXs are very bright The Spitzer IR data show that the majority of the non-nuclear (sources 4, 5, and 25 with LX > 5 × 1039 erg s−1 , marked star-formation activity is confined to the bar and inner spiral with larger circles), and are co-spatial with the ends of the arms (illustrated in red and green), whereas older stellar pop- bar (as previously noted by Brandt et al. 1996). This is con- ulations are spread throughout the disk (illustrated in blue). sistent with models that show that gas can accumulate at the Figure 3 shows the high-resolution 3-color HST/ACS image, tips of bars due to the corotation of the bar structure with where the bar structure, numerous HII regions and dust lanes the disk (Englmaier & Gerhard 1997), thereby creating star- are visible. forming regions where X-ray binaries can form. Other exam- ples of this phenomenon have been observed in the barred 4.1. X-ray Point Source Population galaxies NGC 7771 (Jenkins et al. 2005) and NGC 4303 (Jim´ nez-Bail´ n et al. 2003). e o Figure 4 (top left) shows the DSS optical image of Figure 4 (top right) shows the source positions overlaid on NGC 1672, overlaid with the positions of the 28 X-ray sources
  • 8. 8 Jenkins et al. DSS Spitzer 8µm 1’ 1’ s26 s8 Figure 4.Top left: DSS optical image of NGC1672 with the 28 X-ray source positions marked with blue crosses. Sources with LX > 1039 erg s−1 in the 0.3–10 keV band (i.e. ULXs) in either the XMM-Newton or Chandra observation are marked with red circles, with the 3 brightest (LX > 5 × 1039 erg s−1 ) denoted by larger circles (#4, 5 & 25). Sources that show variability of > 2.5σ between the two observations are also marked with white squares (including sources detected in only one observation). The dotted diamonds denote sources #8 & 26, which are resolved as background galaxies in the optical HST/ACS images; these are shown in the lower panel, where the diamond boxes are 2′′ × 2′′ centered on the X-ray positions. Top right: the Spitzer IRAC continuum-subtracted 8µm image, showing the locations of the X-ray sources with respect to star-forming regions in the galaxy. the Spitzer 8µm image, illustrating the coincidence of many Figure 4 (top left) also denotes variable sources (marked X-ray sources with regions of star-formation in the bar and with white squares). Six sources show significant long-term inner spiral arm regions. We have correlated the X-ray source flux variability between the XMM-Newton and Chandra ob- positions with the HII region catalog of Evans et al. (1996). servations at levels of > 2.5σ; these are sources 1, 4, 6, 8, 21 Taking into account both the absolute astrometric accuracy of and 25. Most notable are the increases in flux in two of the the X-ray and HII region positions (∼1′′ combined) as well as brightest ULXs in the Chandra observations; #4 increases by the measured areas of the HII regions, we associate eleven X- a factor of ∼5 (up to 6.9 × 1039 erg s−1 ), and #25 increases ray sources with HII regions (2, 4, 5, 7, 13, 14, 18, 21, 25, 27, by a factor of ∼3 (up to 9.0 × 1039 erg s−1 ), indicating that and 28). These include the three brightest ULXs, and three the high luminosity of these sources is not due to confusion sources in the circumnuclear ring. of several fainter sources. These flux increases are accompa- We have not performed any complex spectral fitting on the nied by a spectral hardening of source #4, but no significant X-ray sources, as even the brightest are well-fit with simple spectral change in source #25. The other four sources with 2 absorption+powerlaw models, with χν close to 1 (see Ta- spectral fits in both observations show no significant spectral ble 1). The spectra and model fits are shown in Figures 5 change between observations. Another four sources (10, 17, and 6. However, we note that even though this simple model 24 and 27) are only detected in one observation. provides acceptable empirical fits to these data, this is likely To investigate longer-term behavior, in Table 4 we show due to the relatively low photon counts ( 2000 counts, total a comparison between XMM-Newton, Chandra and ROSAT PN+MOS or ACIS-S), and the true underlying spectral shapes HRI soft X-ray luminosities for five sources detected in are likely to be more complex (see Stobbart et al. 2006 for a all three observations. We quote the 0.2–2 keV HRI lu- discussion). minosities from de Naray et al. (2000) for the combined
  • 9. Investigating the nuclear activity of barred spiral galaxies 9 Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) 0.01 S1 S4 S5 2×10−4 5×10−4 10−3 2×10−3 0.01 10−3 10−3 10−4 1.5 1.5 1.5 Ratio Ratio Ratio 1 1 1 0.5 1 2 5 10 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) Energy (keV) 2×10−4 5×10−4 10−32×10−3 5×10−3 Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) S6 S7 S19 5×10−4 10−3 2×10−3 10−3 10−4 2×10−4 2 1.5 1.5 1.5 Ratio Ratio Ratio 1 1 1 0.5 1 2 5 10 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) Energy (keV) 10−4 2×10−4 5×10−4 10−3 2×10−3 Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) S22 S25 0.01 S26 10−3 10−3 10−4 10−4 1.5 1.5 1.5 Ratio Ratio Ratio 1 1 1 0.5 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) 0.5 1 2 5 10 Energy (keV) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) 10−42×10−4 5×10−4 10−32×10−3 S27 S28 10−3 10−4 1.5 1.5 Ratio Ratio 1 1 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) XMM-Newton EPIC spectra of the 11 sources with > 100 net PN or MOS counts. PN data points and power- Figure 5. law+absorption models are shown in green; those of the MOS data are shown in red/black. 1992/1997 dataset (which gives better photon statistics), to- We estimate the number of background X-ray sources in the gether with 0.2–2 keV luminosities derived from the best- D25 area of NGC 1672 using the hard-band (2–10 keV) log fit XMM-Newton and Chandra spectral models corrected for N -log S source distributions from Chandra deep field studies Galactic absorption. Note that we also include #23 (ROSAT (we do not use the soft-band log N -log S since the detec- source X-5), which was originally believed to be coincident tion sensitivity at soft energies will be affected by absorption with a foreground star given the ROSAT positional errors by neutral material in the galactic disk). Using a source de- (∼5′′ ). However, with the Chandra positional accuracy of tection threshold of 12 counts in the 0.3–10 keV band (corre- ∼0.5′′ , we show that this source is not consistent with the sponding to the faintest source detected in the Chandra ob- 2MASS position of the star (04h 45m49.54s , −59◦12′ 54.1′′) servation), and converting this to a 2–10 keV flux for a typi- with an offset of ∼5′′ . In fact, this is the source that shows the cal AGN (∼ 1.5 × 10−15 erg s−1 cm−2 , using Γ = 1.7 and largest long-term variability with Lhigh /Llow = 3.6 over this NHGal = 0.223 × 1021 cm−2 ), the log N -log S relations of ∼10 year period. The remaining sources vary in luminosity Giacconi et al. (2001), Campana et al. (2001) and Bauer et al. by factors of 1 − 3. (2004) all predict between 2–3 background sources in the
  • 10. 10 Jenkins et al. 5×10−4 10−3 2×10−3 5×10−3 0.01 0.02 10−3 2×10−3 5×10−3 0.01 0.02 Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) S1 S4 10−3 S5 5×10−4 2×10−4 1.5 1.5 1.5 Ratio Ratio Ratio 1 1 1 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) 0.5 1 2 5 10 Energy (keV) 5×10−4 10−3 2×10−3 5×10−3 0.01 2×10−4 5×10−4 10−32×10−3 5×10−3 2×10−3 Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) S7 S13 S24 10−3 5×10−4 1.5 1.5 1.5 Ratio Ratio Ratio 1 1 1 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) 0.5 1 2 5 10 Energy (keV) Normalization (count s−1 keV−1) Normalization (count s−1 keV−1) 2×10−3 S25 S28 0.01 10−3 10−3 5×10−4 1.5 1.5 Ratio Ratio 1 1 0.5 1 2 5 10 0.5 1 2 5 10 Energy (keV) Energy (keV) Figure 6. Chandra ACIS-S spectra of the 8 sources with > 100 net counts, together with the powerlaw+absorption models. field. Note that this is in fact an upper limit, since the contours from the continuum-subtracted Spitzer IRAC 8.0µm NGC 1672 source catalog is not corrected for incompleteness. image, which highlights star-formation activity; the diffuse Inspection of the HST/ACS images allows us to identify two emission is spatially correlated with the IR emission, follow- X-ray sources as background galaxies immediately; these are ing the bar/inner spiral arm structure. #26, which appears to be a face-on disk galaxy with a bright A source spectrum was extracted from an elliptical region nucleus, and #8, which looks like an edge-on galaxy with vis- (a, b) = (2.25′ , 1.11′ ) centered on the nucleus with a posi- ible dust lanes seen through the disk of NGC 1672 (see Fig- tion angle of 90◦ . The detected point sources were excluded ure 4, lower panel). As noted in § 3.4.3, source #8 is the only (using regions with twice the radius of the 90% encircled en- extra-nuclear X-ray source with a detected radio counterpart. ergy ellipses), as well as the innermost 20′′ radius circumnu- At the distance of NGC 1672, the 2–10 keV X-ray luminos- clear ring region. The background regions were chosen to be ity (at its brightest in the XMM-Newton observation) would (1) the region on the ACIS-S3 chip outside the D25 radius be LX = 7.9 × 1038 erg s−1 , and the 5 GHz radio luminosity and not containing point sources, and (2) the region on the would be νLν = 2.2 × 1036 erg s−1 . According to the X- ACIS-S1 chip not containing bright point sources. To further ray/radio fundamental plane of Merloni et al. (2003), this is constrain the soft end of the background emission, we also inconsistent with emission from a stellar mass black hole (i.e. used the seven element ROSAT All Sky Survey (RASS) spec- too radio-bright), and supports the hypothesis that this source tral energy distribution (Snowden et al. 1997) from an annulus is a background AGN (see § 5 for further discussion of this 30′ < R < 1◦ around NGC 1672, extracted using the X-ray relation with regards to the nuclear source). background web tool hosted by the HEASARC19 . For each Chandra spectrum, we created a particle background spec- 4.2. Diffuse X-ray Emission trum using the “stowed” data from the appropriate chip and We have used the Chandra observation to study the diffuse mode, scaled to produce the same 10–13 keV band count rate X-ray component of NGC 1672 due to its ∼1′′ spatial resolu- as observed in the ObsID 5932 data. The particle background tion, and hence ease of source subtraction. The morphology spectra were then used as the “background” spectra within of the diffuse emission is illustrated in Figure 2 (d), where the XSPEC, and the spectra of the galaxy and the remainder of the X-ray point sources and central ring region have been masked, 19 http://heasarc.gsfc.nasa.gov/cgi-bin/Tools/xraybg/xraybg.pl and the residual emission adaptively smoothed. Overlaid are