The
                    <i>Chandra</i>
                    Multiwavelength Project: Optical Follow‐up of Serendipitous
                    <i>Chandra</i>
                    Sources

Green, Paul; Silverman, John D.; Cameron, R. A.; Kim, D.‐W.; Wilkes, B. J.; Barkhouse, W. A.; Lacluyzé, A.; Morris, D.; Mossman, Amy E.; Ghosh, H.; Grimes, John; Jannuzi, Buell T.; Tananbaum, H.; Aldcroft, Thomas L.; Baldwin, J. A.; Chaffee, Frederic H.; Dey, Arjun; Dosaj, A.; Evans, Nancy Remage; Fan, Xiaohui; Foltz, C. B.; Gaetz, T. J.; Hooper, E. J.; Kashyap, Vinay; Mathur, S.; McGarry, M. B.; Romero-Colmenero, E.; Smith, M. G.; Smith, Paul S.; Smith, R. C.; Torres, Guillermo; Vikhlinin, A.; Wik, Daniel R.

doi:10.1086/379818

Cited by 78 publications

(17 citation statements)

References 143 publications

(123 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Thus, we include MS1358.4+6245 in our cluster sample with only one detected radio source in the BCG. Yee et al 1996), and/or the Chandra Multi-wavelength Project (ChaMP; Green et al 2004) for 10 of our 11 clusters in this paper.…”

Section: Radio Imagingmentioning

confidence: 99%

See 1 more Smart Citation

X-Ray Point Sources and Radio Galaxies in Clusters of Galaxies

Hart

Stocke

Hallman

2009

ApJ

View full text Add to dashboard Cite

Using Chandra imaging spectroscopy and Very Large Array L-band maps, we have identified radio galaxies at P (1.4 GHz) 3 × 10 23 W Hz −1 and X-ray point sources (XPSs) at L (0.3-8 keV) 10 42 erg s −1 in 11 moderate redshift (0.2 < z < 0.4) clusters of galaxies. Each cluster is uniquely chosen to have a total mass similar to predicted progenitors of the present-day Coma Cluster. Within a projected radius of 1 Mpc we detect 20 radio galaxies and 8 XPSs (three sources are detected in both X-ray and radio) confirmed to be cluster members above these limits. Of these, 75% are detected within 500 kpc (projected) of the cluster center. This result is inconsistent with a random selection from bright, red sequence ellipticals at the >99.999% level. We suggest that these active galactic nuclei (AGNs) are triggered somehow by the intracluster medium (ICM), perhaps similar to the Bondi accretion model of Allen et al. All but one of the XPSs are hosted by luminous ellipticals which otherwise show no other evidence for AGN activity. These objects are unlikely to be highly obscured AGN since there is no evidence for large amounts of X-ray or optical absorption. One XPS, in addition to possessing a pure absorption-line optical spectrum, has a large excess of light blueward of the Ca ii H&K break that could be nonthermal emission; a second XPS host galaxy probably has excess blue light. The most viable model for these sources are low-luminosity BL Lac Objects, similar to the high-energy-peaked BL Lacs (HBLs) discovered in abundance in serendipitous X-ray surveys. The expected numbers of lower luminosity FR 1 radio galaxies and HBLs in our sample converge to suggest that very deep radio and X-ray images of rich clusters will detect AGN (either X-ray or radio emitting or both) in a large fraction of bright elliptical galaxies in the inner 500 kpc. Because both the radio galaxies and the XPSs possess relativistic jets, they (and, by extension, the entire radio luminosity function) can inject heat into the ICM. Using the most recent scalings of P jet ∝ L 0.5 r from Bîrzan et al., radio sources weaker than our luminosity limit probably contribute the majority of the heat to the ICM. Also, because these heat sources move around the cluster, AGN heating is distributed rather evenly. If a majority of ICM heating is due to large numbers of low-power radio sources, triggered into activity by the increasing ICM density as they move inward, this may be the feedback mechanism necessary to stabilize cooling in cluster cores.

show abstract

Section: Radio Imagingmentioning

confidence: 99%

“…This work made use of images and/or data products provided by the Chandra Multi-wavelength Project (ChaMP; Green et al 2004) …”

mentioning

confidence: 99%

X-Ray Point Sources and Radio Galaxies in Clusters of Galaxies

Hart

Stocke

Hallman

2009

ApJ

View full text Add to dashboard Cite

show abstract

“…Using Chandra X-ray imaging, in Section 3 we study the high-energy SEDs of binary quasars (Section 3.1) and how they compare (in Section 3.2) to a subset of QSOs imaged in X-rays by Chandra as part of the Chandra Multiwavelength Project (ChaMP; Green et al 2004Green et al , 2009. In Section 4, we present deep IR imaging we obtained at Mt Hopkins using the SAO Wide-field InfraRed Camera (SWIRC) on the 6.5 m MMT to further examine the SEDs of binary QSOs.…”

Section: Introductionmentioning

confidence: 99%

A Multiwavelength Study of Binary Quasars and Their Environments

Green

Myers

Barkhouse

et al. 2011

ApJ

View full text Add to dashboard Cite

We present Chandra X-ray imaging and spectroscopy for 14 quasars in spatially resolved pairs targeted as part of a complete sample of binary quasars with small transverse separations drawn from Sloan Digital Sky Survey (SDSSDR6) photometry. We measure the X-ray properties of all 14 QSOs, and study the distribution of X-ray and optical-to-X-ray power-law indices in these binary quasars. We find no significant difference when compared with large control samples of isolated quasars, true even for SDSS J1254+0846, discussed in detail in a companion paper, which clearly inhabits an ongoing, pre-coalescence galaxy merger showing obvious tidal tails. We present infrared photometry from our observations with SAO Wide-field InfraRed Camera at the MMT, and from the Wide-field Infrared Survey Explorer Preliminary Data Release, and fit simple spectral energy distributions to all 14 QSOs. We find preliminary evidence that substantial contributions from star formation are required, but possibly no more so than for isolated X-ray-detected QSOs. Sensitive searches of the X-ray images for extended emission and the optical images for optical galaxy excess show that these binary QSOs-expected to occur in strong peaks of the dark matter distribution-are not preferentially found in rich cluster environments. While larger binary QSO samples with richer far-IR and submillimeter multiwavelength data might better reveal signatures of merging and triggering, optical color selection of QSO pairs may be biased against such signatures. X-ray and/or variability selection of QSO pairs, while challenging, should be attempted. We present in an Appendix a primer on X-ray flux and luminosity calculations.

show abstract

“…CX10c and CX10f are above the main sequence. e Ratio of X-ray to optical (R 625 ) flux, using log (f X /f r ) = log f X + 5.67 + 0.4R 625 (Green et al 2004); f X is derived in the 0.5-2 keV band. f The tentative classifications of multiple sources are valid only if the counterparts are true.…”

Section: Sources Inside the Half-mass Radiusmentioning

confidence: 99%

CHANDRAANDHSTSTUDIES OF THE X-RAY SOURCES IN GALACTIC GLOBULAR CLUSTER M92

Lu¹,

Kong²,

Verbunt³

et al. 2011

ApJ

View full text Add to dashboard Cite

We present the analysis of two observations of M92 taken with the Chandra X-Ray Observatory. We combined the two data sets with a total exposure of ∼52 ks. With the combined observation, we detected 10 X-ray sources inside the half-mass radius (1. 02), five of which are inside the core radius (0. 26) of M92. The luminosities of the 10 sources are roughly within the range of 10 30 -10 32 erg s −1 assuming cluster memberships. The background estimation suggests 7-8 cluster members and 2-3 background galaxies in M92. We identified the 10 sources by using Hubble Space Telescope Advanced Camera for Surveys observations of M92. Based on the X-ray and optical characteristics, we classified 4-5 possible candidates for cataclysmic variables within the half-mass radius. We discussed the possible formation mechanisms of the X-ray sources in M92 by comparing the predicted X-ray source number and observational results. Under the assumption that the number of X-ray sources scales with the encounter rate and the mass of the globular cluster, we expected eight X-ray sources formed from dynamical interactions and four from primordial binaries inside M92, which is consistent with the background estimation and comparable with the observational results. We therefore suggest that the X-ray sources in M92 may be contributed from both dynamical origin and primordial binaries.

show abstract

The Chandra Multiwavelength Project: Optical Follow‐up of Serendipitous Chandra Sources

Cited by 78 publications

References 143 publications

X-Ray Point Sources and Radio Galaxies in Clusters of Galaxies

X-Ray Point Sources and Radio Galaxies in Clusters of Galaxies

A Multiwavelength Study of Binary Quasars and Their Environments

CHANDRAANDHSTSTUDIES OF THE X-RAY SOURCES IN GALACTIC GLOBULAR CLUSTER M92

Contact Info

Product

Resources

About