Erratum: “Infrared Counterparts to<i>Chandra</i>X‐Ray Sources in the Antennae” (ApJ, 658, 319 [2007])

Clark, David M.; Eikenberry, S. S.; Brandl, Bernhard R.; Wilson, J. C.; Carson, J.; Henderson, C.; Hayward, T. L.; Barry, D. J.; Ptak, A.; Colbert, E. J. M.

doi:10.1086/521221

Cited by 3 publications

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“…Compact objects tend to be associated with massive star formation, which some theories suggest is predominant in young stellar clusters (Lada & Lada 2003). In previous work on the Antennae we find a close association between compact objects and clusters, identifying 15 possible IR counterparts to X-ray sources (Clark et al 2007). Many of these counterparts reside in the spiral arms and 'bridge' region of the Antennae -locations predominant in massive star formation.…”

Section: Introductionmentioning

confidence: 50%

“…Those X-ray sources without counterparts could be compact objects that escaped their parent cluster or remained behind after their cluster dissolved. In Clark et al (2007) we suggest a third possibility, that some X-ray sources do have counterparts, but these are too faint to see in the IR images.…”

Section: Introductionmentioning

confidence: 82%

“…In the new catalogue of X-ray sources, Zezas et al (2006) revised the X-ray source positions and the new positions differ by 0.2 ± 0.4 arcsec in R.A. and 0.6 ± 1.8 arcsec in Dec as compared to those coordinates listed in Zezas et al (2002). Considering we are searching for IR counterparts within 1 arcsec of an X-ray source position (see below), we adjusted our initial frame-tie (Clark et al 2007) between the WIRC, IR Ks-band image and the X-ray sources listed in Zezas et al (2002), to account for the new, X-ray coordinates listed in Zezas et al (2006). This modification to the initial frame-tie yielded the same rms positional uncertainty, ∼ 0.5 arcsec.…”

Section: Infrared and Optical Imagingmentioning

confidence: 99%

“…

We use WIRC, IR images of the Antennae (NGC 4038/4039) together with the extensive catalogue of 120 X-ray point sources (Zezas et al 2006) to search for counterpart candidates. Using our proven frame-tie technique, we find 38 X-ray sources with IR counterparts, almost doubling the number of IR counterparts to X-ray sources first identified in Clark et al (2007). In our photometric analysis, we consider the 35 IR counterparts that are confirmed star clusters.

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confidence: 95%

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Multiwavelength study of Chandra X-ray sources in the Antennae

Clark

Eikenberry

Brandl

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We use Wide-field InfraRed Camera (WIRC) infrared (IR) images of the Antennae (NGC 4038/ 4039) together with the extensive catalogue of 120 X-ray point sources to search for counterpart candidates. Using our proven frame-tie technique, we find 38 X-ray sources with IR counterparts, almost doubling the number of IR counterparts to X-ray sources that we first identified. In our photometric analysis, we consider the 35 IR counterparts that are confirmed star clusters. We show that the clusters with X-ray sources tend to be brighter, K s ≈ 16 mag, with (J− K s ) = 1.1 mag.We then use archival Hubble Space Telescope (HST) images of the Antennae to search for optical counterparts to the X-ray point sources. We employ our previous IR-to-X-ray frame-tie as an intermediary to establish a precise optical-to-X-ray frame-tie with <0.6 arcsec rms positional uncertainty. Due to the high optical source density near the X-ray sources, we determine that we cannot reliably identify counterparts. Comparing the HST positions to the 35 identified IR star cluster counterparts, we find optical matches for 27 of these sources. Using Bruzual-Charlot spectral evolutionary models, we find that most clusters associated with an X-ray source are massive, and young, ∼10 6 yr.

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Section: Introductionmentioning

confidence: 50%

Section: Introductionmentioning

confidence: 82%

Section: Infrared and Optical Imagingmentioning

confidence: 99%

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confidence: 95%

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Multiwavelength study of Chandra X-ray sources in the Antennae

Clark

Eikenberry

Brandl

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…We note that of the 19 X-ray sources with counterparts, two are the nuclei , one is a background quasar (Clark et al 2005), and two share the same IR counterpart. Therefore, in this paper we only consider the 15 IR counterparts (of the original 19) that are star clusters in the Antennae.…”

Section: Infrared Imagesmentioning

confidence: 87%

A First Estimate of the X‐Ray Binary Frequency as a Function of Star Cluster Mass in a Single Galactic System

Clark¹,

Eikenberry²,

Brandl³

et al. 2008

ApJ

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We use the previously identified 15 infrared star cluster counterparts to X-ray point sources in the interacting galaxies NGC 4038/4039 (the Antennae) to study the relationship between total cluster mass and X-ray binary number. This significant population of X-Ray/ IR associations allows us to perform, for the first time, a statistical study of X-ray point sources and their environments. We define a quantity, , relating the fraction of X-ray sources per unit mass as a function of cluster mass in the Antennae. We compute cluster mass by fitting spectral evolutionary models to K s luminosity. Considering that this method depends on cluster age, we use four different age distributions to explore the effects of cluster age on the value of and find it varies by less than a factor of 4. We find a mean value of for these different distributions of ¼ 1:7 ; 10 À8 M À1 with ¼ 1:2 ; 10 À8 M À1 . Performing a 2 test, we demonstrate could exhibit a positive slope, but that it depends on the assumed distribution in cluster ages. While the estimated uncertainties in are factors of a few, we believe this is the first estimate made of this quantity to ''order of magnitude'' accuracy. We also compare our findings to theoretical models of open and globular cluster evolution, incorporating the X-ray binary fraction per cluster.

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SPITZER-IRS STUDY OF THE ANTENNAE GALAXIES NGC 4038/39

Brandl¹,

Snijders²,

Brok³

et al. 2009

ApJ

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103

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Using the Infrared Spectrograph on the Spitzer Space Telescope, we observed the Antennae galaxies obtaining spectral maps of the entire central region and high signal-to-noise 5 − 38µm spectra of the two galactic nuclei and six infrared-luminous regions.The total infrared luminosity of our six IR peaks plus the two nuclei is L IR = 3.8·10 10 L ⊙ , with their derived star formation rates ranging between 0.2 and 2 M ⊙ /yr, with a total of 6.6 M ⊙ /yr. None of the typical mid-infrared tracers of AGN activity is detected in either nucleus of the system, excluding the presence of an dust enshrouded accretion disk. The hardest and most luminous radiation originates from two compact clusters in the southern part of the overlap region, which also have the highest dust temperatures. PAH emission and other tracers of softer radiation are spatially extended throughout and beyond the overlap region, but regions with harder and intenser radiation field show a reduced PAH strength.The strong H 2 emission is rather confined around the nucleus of NGC 4039, where shocks appear to be the dominant excitation mechanism, and the southern part of the overlap region, where it traces the most recent starburst activity. The luminosity ratio between the warm molecular gas (traced by the H 2 lines) and the total far-IR emission is ∼ 1.6 · 10 −4 , similar to that found in many starburst and ULIRGs. The total mass of warm H 2 in the Antennae is 2.5 · 10 7 M ⊙ , with a fraction of warm to total H 2 gas mass of about 0.35%. The average warm H 2 temperature is 302 ± 26 K and appears anti-correlated with the radiation field hardness, possibly due to an evolution of the PDR morphology. The previously reported tight correlation between the H 2 and PAH emission was not found but higher total PAH emission to continuum ratios were found in PDRs with warmer gas.

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Erratum: “Infrared Counterparts toChandraX‐Ray Sources in the Antennae” (ApJ, 658, 319 [2007])

Abstract: In equation (2), we incorrectly labeled one of the variables. Equations (1) and (2) should read:These equations were used only to explain our image frame-tie method, and this change does not affect our results.

Cited by 3 publications

References 0 publications

Multiwavelength study of Chandra X-ray sources in the Antennae

Multiwavelength study of Chandra X-ray sources in the Antennae

A First Estimate of the X‐Ray Binary Frequency as a Function of Star Cluster Mass in a Single Galactic System

SPITZER-IRS STUDY OF THE ANTENNAE GALAXIES NGC 4038/39

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