Testing the connection between the X-ray and submillimetre source populations using Chandra

Fabian, A. C.; Smail, Ian; Iwasawa, K.; Allen, S. W.; Blain, A. W.; Crawford, C. S.; Ettori, S.; Ivison, R. J.; Johnstone, R. M.; Kneib, Jean-Paul; Wilman, R. J.

doi:10.1046/j.1365-8711.2000.03621.x

Cited by 114 publications

(78 citation statements)

References 28 publications

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“…The XMM soft X-ray (rest frame hard X-ray) upper limit suggests L 2−10kev /L bol 10 −3 and excludes an unobscured type 1 AGN. In the submillimetre to X-ray spectral index vs. redshift diagram of Fabian et al (2000), the index limit of >1.4 places Lockman 850.1 even beyond Compton-thick obscured AGN with properties similar to NGC 6240, for all plausible redshifts. If Lockman 850.1 hosts an AGN, it must be weak and/or heavily obscured.…”

Section: Discussionmentioning

confidence: 93%

The extended counterpart of submm source Lockman 850.1

Lutz

Dunlop

Almaini

et al. 2001

A&A

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Abstract. The IRAM Plateau de Bure mm interferometer and deep K-band imaging have been used to identify the brightest submm source detected in the Lockman field of the UK 8 mJy SCUBA survey. The near infrared counterpart is an extended (20-30 kpc), clumpy, and extremely red object. The spectral energy distribution suggests it to be a dusty star forming object at a redshift of about 3 (2-4). Its star formation rate and nearinfrared properties are consistent with Lockman 850.1 being a massive elliptical in formation.

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Section: Discussionmentioning

confidence: 93%

The extended counterpart of submm source Lockman 850.1

Lutz

Dunlop

Almaini

et al. 2001

A&A

Self Cite

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“…The + sign identifies sources detected at 7 µm but not at 15 µm. If the ID number of a source is enclosed within a square then the source has been detected at X-ray wavelengths in Chandra data (Fabian et al 2000;Wilman et al 2000a). If the ID number of a source is enclosed within a circle then the source has been detected at submm wavelengths with SCUBA Cowie et al 2002).…”

Section: Results -Number Counts and Source Propertiesmentioning

confidence: 99%

“…The -sign identifies sources detected at 15 µm but not at 7 µm. If the ID number of a source is enclosed within a square then the source has been detected at X-ray wavelengths in Chandra data (Fabian et al 2000;Wilman et al 2000a).…”

Section: Corrections Applied In Deriving the Countsmentioning

confidence: 99%

K$_{\mbox{\fontsize{12pt}{14pt}\selectfont{\textit{s}}}}$-band luminosity function of thez= 1.237 cluster of galaxies RDCS J1252.9-2927

Toft¹,

Mainieri²,

Rosati³

et al. 2004

A&A

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Abstract. ESA's Infrared Space Observatory (ISO) was used to perform a deep survey with ISOCAM through three massive gravitationally lensing clusters of galaxies. The total area surveyed depends on source flux, with nearly seventy square arcminutes covered for the brighter flux levels in maps centred on the three clusters Abell 370, Abell 2218 and Abell 2390. We present maps and photometry at 6.7 µm (hereafter 7 µm) and 14.3 µm (hereafter 15 µm), showing a total of 145 mid-infrared sources and the associated source counts. At 15 µm these counts reach the faintest level yet recorded. Almost all of the sources have been confirmed on more than one infrared map and all are identified with counterparts in the optical or near-infrared. Detailed models of the three clusters have been used to correct for the effects of gravitational lensing on the background source population. Lensing by the clusters increases the sensitivity of the survey, and the weakest sources have lensing corrected fluxes of 5 and 18 µJy at 7 and 15 µm, respectively. Roughly 70% of the 15 µm sources are lensed background galaxies. Of sources detected only at 7 µm, 95% are cluster galaxies for this sample. Of fifteen SCUBA sources within the mapped regions of the three clusters seven were detected at 15 microns. The redshifts for five of these sources lie in the range 0.23 to 2.8, with a median value of 0.9. Flux selected subsets of the field sources above the 80% and 50% completeness limits were used to derive source counts to a lensing corrected sensitivity level of 30 µJy at 15 µm, and 14 µJy at 7 µm. The source counts, corrected for the effects of completeness, contamination by cluster sources and lensing, confirm and extend earlier findings of an excess by a factor of ten in the 15 µm population with respect to source models with no evolution. The observed mid-infrared field sources occur mostly at redshifts between 0.4 and 1.5. For the counts at 7 µm, integrating in the range 14 µJy to 460 µJy, we resolve (0.49± 0.2)×10 −9 W m −2 sr −1 of the infrared background light into discrete sources. At 15 µm we include the counts from other extensive ISOCAM surveys to integrate over the range 30 µJy to 50 mJy, reaching two to three times deeper than the unlensed surveys to resolve (2.7 ± 0.62) × 10 −9 W m −2 sr −1 of the infrared background light. These values correspond to 10% and 55%, respectively, of the upper limit to the infrared background light, derived from photon-photon pair production of the high energy gamma rays from BL-Lac sources on the infrared background photons. However, the recent detections of TeV gamma rays from the z = 0.129 BL Lac H1426+428 suggest that the value for the 15 µm background reported here is already sufficient to imply substantial absorption of TeV gamma rays from that source.Key words. surveys -galaxies: clusters: individual: Abell 370 -galaxies: clusters: individual: Abell 2218 -galaxies: clusters: individual: Abell 2390 -gravitational lensing -infrared: galaxiesSend offprint requests to: L. Metcalfe, e-mail: lmetca...

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“…An important diagnostic is being offered by observations of the hard X-ray flux, since starbursts are weaker X-ray emitters than any kinds of AGNs. The Chandra X-ray observatory has performed several deep investigations of the high-z SCUBA population (Fabian et al 2000;Hornschemeier et al 2000;and Barger et al 2001). Only a very small percentage of the objects turn out to be in common, the two classes of sources being largely orthogonal.…”

Section: Agn Contributions To the Source Energeticsmentioning

confidence: 99%

A long-wavelength view on galaxy evolution from deep surveys by the Infrared Space Observatory

Franceschini

Aussel

Césarsky

et al. 2001

A&A

200

309

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Abstract.We discuss the constraints set on galaxy evolution by a variety of data from deep extragalactic surveys performed in the mid-IR and far-IR with the Infrared Space Observatory and with millimetric telescopes at longer wavelengths. These observations indicate extremely high rates of evolution for IR galaxies, exceeding those measured for galaxies at other wavelengths and comparable or larger than the rates observed for quasars. We also match the modelled integrated emission by IR galaxies at any redshifts with the observed spectral intensity of the extragalactic IR background (CIRB), as a further constraint. The multi-wavelength statistics on IR galaxies can be reconciled with each other by assuming for the bulk of the population spectral energy distributions (SED) as typical for starbursts, which we take as an indication that stellar (rather than AGN, see also Fadda et al. 2001) activity powers IR emission by faint galaxies. According to our model and following the analysis of Elbaz et al. (2001), the deep ISO surveys at 15 µm may have already resolved more than 50% of the bolometric CIRB intensity: the faint ISO 15 µm source samples, relatively easy to identify in deep optical images , can then allow to investigate the origin of the CIRB background. From our fits to the observed optical-IR SEDs, these objects appear to mostly involve massive galaxies hosting luminous starbursts (SF R ∼ 100 M /yr). The evolutionary scheme we infer from these data considers a bimodal star formation (SF), including a phase of long-lived quiescent SF, and enhanced SF taking place during transient events recurrently triggered by interactions and merging. We interpret the strong observed evolution as an increase with z of the rate of interactions between galaxies (density evolution) and an increase of their IR luminosity due to the more abundant fuel available in the past (luminosity evolution): both factors enhance the probability to detect a galaxy during the "active" phase at higher z. Very schematically, we associate the origin of the bulk of the optical/NIR background to the quiescent evolution, while the CIRB is interpreted as mostly due the dusty starburst phase. The latter possibly leads to the formation of galaxy spheroids, when the dynamical events triggering the starburst re-distribute already present stellar populations. The large energy contents in the CIRB and optical backgrounds are not easily explained, considering the moderate efficiency of energy generation by stars: a top-heavy stellar IMF associated with the starburst phase (and compared with a more standard IMF during the quiescent SF) would alleviate the problem. The evolution of the IR emissivity of galaxies from the present time to z ∼ 1 is so strong that the combined set of constraints by the observed z-distributions and the CIRB spectrum impose it to turn-over at z > 1: scenarios in which a dominant fraction of stellar formation occurs at very high-z are not supported by our analysis.

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Testing the connection between the X-ray and submillimetre source populations using Chandra

Cited by 114 publications

References 28 publications

The extended counterpart of submm source Lockman 850.1

The extended counterpart of submm source Lockman 850.1

K$_{\mbox{\fontsize{12pt}{14pt}\selectfont{\textit{s}}}}$-band luminosity function of thez= 1.237 cluster of galaxies RDCS J1252.9-2927

A long-wavelength view on galaxy evolution from deep surveys by the Infrared Space Observatory

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