A DEEP
                    <i>CHANDRA</i>
                    ACIS SURVEY OF M83

Long, Knox S.; Küntz, K. D.; Blair, William P.; Godfrey, L.; Plucinsky, Paul P.; Soria, Roberto; Stockdale, C. J.; Winkler, P. F.

doi:10.1088/0067-0049/212/2/21

Cited by 66 publications

(114 citation statements)

References 75 publications

(163 reference statements)

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“…For our source with the angular extent of NGC 45, we would expect to detect approximately 11 SNRs, but the SFR of M83 is an order of magnitude greater than that of NGC 45 (for example, Kaisinia 2013 and estimate the SFRs of NGC 45 and M83 to be 0.55 and 2.82 M  yr −1 , respectively, based on Hα fluxes of the galaxies). Assuming that the SNR detection rate of a galaxy scales in proportion to its SFR, from the estimate of Long et al (2014) we may expect to detect only one SNR in the X-ray in NGC 45, which broadly matches our result. The low SFR of NGC 45 (as calculated and discussed in Section 4) suggests that both the sheer number of SNRs and the number of luminous SNRs is probably much lower than in galaxies like the Milky Way and NGC 7793 that have much higher SFRs.…”

Section: Counterparts To Discrete X-ray Sources Detected At Other Wavsupporting

confidence: 86%

“…As noted in that paper, only about ten Galactic SNRs are known to have X-ray luminosities that exceed the limiting luminosity of our observation 14 , though comparisons with the Galactic SNR population need to be tempered by the fact that significant absorption along Galactic lines of sight causes many soft X-ray emitting sources like SNRs to remain undetected. In their study of X-ray emission from SNRs in the galaxy M83, Long et al (2014) estimated a surface area distribution of the SNRs to be approximately 1000 SNRs per square degree at a flux limit corresponding to that attained by our observation of NGC 45. For our source with the angular extent of NGC 45, we would expect to detect approximately 11 SNRs, but the SFR of M83 is an order of magnitude greater than that of NGC 45 (for example, Kaisinia 2013 and estimate the SFRs of NGC 45 and M83 to be 0.55 and 2.82 M  yr −1 , respectively, based on Hα fluxes of the galaxies).…”

Section: Counterparts To Discrete X-ray Sources Detected At Other Wavmentioning

confidence: 57%

“…Specifically, these obstacles include considerable uncertainties in the distances to Galactic SNRs and significant absorption along the lines of sight to these sources (particularly at short wavelengths such as visible and X-ray), which limit thorough studies of Galactic SNRs to only those sources located in the neighborhood of the Sun (see Pannuti et al 2007 for a more detailed review). Examples of papers that have provided detailed analysis of X-ray emission from samples of extragalactic SNRs as detected by Chandra include Long et al (2010Long et al ( , 2014 who considered the SNRs located in the nearby spiral galaxies M33 and M83, respectively. Our prior analyses of Chandra observations of SNRs in nearby galaxies include the study of five galaxies in a flux-limited sample (Pannuti et al 2007) as well as the study of the resident SNRs in NGC 7793 (Pannuti et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

Pannuti

Swartz²,

Laine

et al. 2015

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We present an analysis of high angular resolution observations made in the X-ray and the radio with the Chandra X-ray Observatory and the Karl Jansky Very Large Array (VLA), respectively, of the nearby spiral galaxy NGC 45. This galaxy is the third that we have considered in a study of the supernova remnant (SNR) populations of nearby spiral galaxies and the present work represents the first detailed analysis of the discrete X-ray and radio source populations of this galaxy. We analyzed data sets from the three pointed observations made of this galaxy with Chandra along with a merged data set obtained from combining these data sets: the total effective exposure time of the merged data set is 63515 s. A total of 25 discrete X-ray sources are found in the entire field of view of the ACIS-S3 chip, with 16 sources found within the visual extent of the galaxy. We estimate that as many as half of the sources detected in the entire field of view of the ACIS-S3 chip and seven of the sources detected in the optical extent of NGC 45 may be background sources. We analyzed the spectral properties of the discrete X-ray sources within the galaxy and conclude that the majority of these sources are X-ray binaries. We have searched for counterparts at different wavelengths to the discrete X-ray sources and we find two associations: one with a star cluster and the other with a background galaxy. We have found one source that is clearly variable within one observation and seven that are seen to vary from one observation to another. We also conduct a photometric analysis to determine the near-infrared fluxes of the discrete X-ray sources in Spitzer Infrared Array Camera channels. We constructed a cumulative luminosity function of the discrete X-ray sources seen toward NGC 45: taking into account simultaneously the luminosity function of background sources, the fitted slope of the cumulative luminosity function Γ = -1.3 1.6 0.7 -+ (all error bounds correspond to 90% confidence intervals). The VLA observations reveal seven discrete radio sources: we find no overlaps between these sources and the X-ray detected sources. Based on their measured spectral indices and their locations with respect to the visible extent of NGC 45, we classify one source as a candidate radio SNR associated with the galaxy and the others as likely background galaxies seen in projection toward NGC 45. Finally, we discuss the properties of a background cluster of galaxies (denoted as CXOU J001354.2-231254.7) seen in projection toward NGC 45 and detected by the Chandra observations. The fit parameters to the extracted Chandra spectra of this cluster are a column density N H = 0.07 (<0.14) × 10 22 cm −2 , a temperature kT = 4.22 1.42 2.08 -+ keV, an abundance Z = 0.30(<0.75) relative to solar and a redshift z = 0.28 ± 0.14. From the fit parameters we derive an electron number density n e = 4(±1) × 10 −3 cm −3 , an unabsorbed X-ray luminosity L 0.5 7.0 keV-8.77(±0.96) × 10 43 erg s −1 for the cluster and an X-ray emitting mass M = 2.32(±1.75) × 10 12 M  .

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Section: Counterparts To Discrete X-ray Sources Detected At Other Wavsupporting

confidence: 86%

Section: Counterparts To Discrete X-ray Sources Detected At Other Wavmentioning

confidence: 57%

Section: Introductionmentioning

confidence: 99%

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CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

Pannuti

Swartz²,

Laine

et al. 2015

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“…M83 has an extended HI disk that is detected to R > 50 kpc, with warped and filamentary structure suggestive of interactions with a companion (Miller et al 2009, Heald et al 2016). In the inner disk, Miller et al Chandra X-ray Observatory observations reveal diffuse, soft X-ray emission that traces the nucleus and spiral arms of M83 (Soria & Wu 2002Long et al 2014). In the starburst nucleus, the diffuse, hot gas has a temperature of T ∼ 7 × 10 6 K, a redshifted velocity of ∼ 7000 km s −1 , and abundances consistent with enrichment by Type-II supernovae and stellar winds from Wolf-Rayet stars (Soria & Wu 2002).…”

Section: Introductionmentioning

confidence: 99%

Detection of Extraplanar Diffuse Ionized Gas in M83*

Boettcher

Gallagher

Zweibel

2017

ApJ

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We present the first kinematic study of extraplanar diffuse ionized gas (eDIG) in the nearby, face-on disk galaxy M83 using optical emission-line spectroscopy from the Robert Stobie Spectrograph on the Southern African Large Telescope. We use a Markov Chain Monte Carlo method to decompose the [NII]λλ6548, 6583, Hα, and [SII]λλ6717, 6731 emission lines into HII region and diffuse ionized gas emission. Extraplanar, diffuse gas is distinguished by its emission-line ratios ([NII]λ6583/Hα ∼ > 1.0) and its rotational velocity lag with respect to the disk (∆v = −24 km s −1 in projection). With interesting implications for isotropy, the velocity dispersion of the diffuse gas, σ = 96 km s −1 , is a factor of a few higher in M83 than in the Milky Way and nearby, edge-on disk galaxies. The turbulent pressure gradient is sufficient to support the eDIG layer in dynamical equilibrium at an electron scale height of h z = 1 kpc. However, this dynamical equilibrium model must be finely tuned to reproduce the rotational velocity lag. There is evidence of local bulk flows near star-forming regions in the disk, suggesting that the dynamical state of the gas may be intermediate between a dynamical equilibrium and a galactic fountain flow. As one of the first efforts to study eDIG kinematics in a face-on galaxy, this study demonstrates the feasibility of characterizing the radial distribution, bulk velocities, and vertical velocity dispersions in low-inclination systems.

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“…For candidates in the outer galaxy, plus a few low-surface-brightness -7 -ones within the WFC3 footprint, we used the Magellan images instead, adjusted for seeing. Column 6 gives the galactocentric distance; and column 7 notes objects that were detected in the Chandra ACIS X-ray survey by Long et al (2014). Column 8 gives the mask and slitlet number used for extracting the one-dimensional spectra.…”

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confidence: 99%

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗

Winkler

Blair

Long

2017

ApJ

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We report the results from a spectrophotometric study sampling the 300 candidate supernova remnants (SNRs) in M83 identified through optical imaging with Magellan/IMACS and HST/WFC3. Of the 118 candidates identified based on a high [S II] λλ 6716,6731 to Hα emission ratio, 117 show spectroscopic signatures of shock-heated gas, confirming them as SNRs-the largest uniform set of SNR spectra for any galaxy. Spectra of 22 objects with a high [O III] λ 5007 to Hα emission ratio, selected in an attempt to identify young ejecta-dominated SNRs like Cas A, reveal only one (previously reported) object with the broad ( 1000 km s −1 ) emission lines characteristic of ejecta-dominated SNRs, beyond the known SN1957D remnant. The other 20 [O III]-selected candidates include planetary nebulae, compact H II regions, and one background QSO. Although our spectroscopic sample includes 22 SNRs smaller than 11 pc, none of the other objects shows broad emission lines; instead their spectra stem from relatively slow (∼ 200 km s −1 ) radiative shocks propagating into the metal-rich interstellar medium of M83. With six SNe in the past century, one might expect more of M83's small-diameter SNRs to show evidence of ejecta; this appears not to be the case. We attribute their absence to several factors, including that SNRs expanding into a dense medium evolve quickly to the ISM-dominated phase, and that SNRs expanding into regions already evacuated by earlier SNe are probably very faint.

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A DEEP CHANDRA ACIS SURVEY OF M83

Cited by 66 publications

References 75 publications

CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

Detection of Extraplanar Diffuse Ionized Gas in M83*

A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗

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A DEEP CHANDRA ACIS SURVEY OF M83

Cited by 66 publications

References 75 publications

CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

CHANDRAAND VERY LARGE ARRAY OBSERVATIONS OF THE NEARBY Sd GALAXY NGC 45

Detection of Extraplanar Diffuse Ionized Gas in M83*

A Spectroscopic Study of the Rich Supernova Remnant Population in M83∗

Contact Info

Product

Resources

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A Spectroscopic Study of the Rich Supernova Remnant Population in M83^∗