A <i>Chandra</i> observation of the <i>z</i>= 2.285 galaxy FSC 10214+4724: evidence for a Compton-thick quasar?

Alexander, D. M.; Chartas, G.; Bauer, F. E.; Brandt, W. N.; Simpson, Chris; Vignali, C.

doi:10.1111/j.1745-3933.2005.08621.x

Cited by 26 publications

(38 citation statements)

References 59 publications

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“…We also include CDF-202, a X ray detected heavily absorbed type 2 QSO at z = 3.7 (Norman et al 2002), and Mrk 231, a BAL QSO which is heavily absorbed in the X rays and is hosted by a powerful starburst galaxy. We do not consider F 10214+4724 because its X ray spectrum is likely dominated by starburst emission (Alexander et al 2005b). The absorption-corrected hard X ray luminosities of CDFS-263, CXOJ1417, and CDF-202 are 7.6 × 10 44 , 2.4 × 10 44 , and 3.3 × 10 44 erg s −1 , respectively.…”

Section: Comparison With Other High-z Qsosmentioning

confidence: 99%

Obscured and powerful AGN and starburst activities at z ~ 3.5

Polletta¹,

Omont²,

Berta³

et al. 2008

A&A

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Aims. Short phases of coeval powerful starburst and AGN activity during the lifetimes of the most massive galaxies are predicted by various models of galaxy formation and evolution. In spite of their recurrence and high luminosity, such events are rarely observed. Finding such systems, understanding their nature, and constraining their number density can provide key constraints to galaxy evolutionary models and insights into the interplay between starburst and AGN activities. Methods. We report the discovery of two sources at z = 3.867 and z = 3.427 that exhibit both powerful starburst and AGN activities. They benefit from multi-wavelength data from radio to X rays from the CFHTLS-D1/SWIRE/XMDS surveys. Follow-up optical and near-infrared spectroscopy, and millimeter IRAM/MAMBO observations are also available. We performed a multi-wavelength analysis of their spectral energy distributions with the aim of understanding the origin of their emission and constraining their luminosities. A comparison with other composite systems at similar redshifts from the literature is also presented. Results. The AGN and starburst bolometric luminosities are ∼1013 L . The AGN emission dominates at X ray, optical, mid-infrared wavelengths, and probably also in the radio. The starburst emission dominates in the far-infrared. The estimated star formation rates range from 500 to 3000 M /yr. The AGN near-infrared and X ray emissions are heavily obscured in both sources with an estimated dust extinction A V ≥ 4, and Compton-thick gas column densities. The two sources are the most obscured and most luminous AGNs detected at millimeter wavelengths currently known. Conclusions. The sources presented in this work are heavily obscured QSOs, but their properties are not fully explained by the standard AGN unification model. In one source, the ultraviolet and optical spectra suggest the presence of outflowing gas and shocks, and both sources show emission from hot dust, most likely in the vicinity of the nucleus. Evidence of moderate, AGN-driven radio activity is also found in both sources. Based on the estimated stellar and black hole masses, the two sources lie on the local M BH −M bulge relation. To remain on this relation as they evolve, their star formation rate has to decrease or stop. Our results support evolutionary models that invoke radio feedback such as the star formation quenching mechanism, and suggest that such a mechanism might play a major role also in powerful AGNs.

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Section: Comparison With Other High-z Qsosmentioning

confidence: 99%

Obscured and powerful AGN and starburst activities at z ~ 3.5

Polletta¹,

Omont²,

Berta³

et al. 2008

A&A

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“…These two are inconsistent with each other at a 95.4 per cent level. Wilman et al (2003) and Alexander et al (2005) found evidence of soft X-ray emission associated with HyLIRGs and ULIRGs, and they suggested that its origin be thermal emission from star formation. However, the X-ray emission detected in these studies was significantly softer (kT ∼ 0.3 keV) and of lower luminosity (∼10 42 erg s −1 ) than that detected here.…”

Section: Origin Of the Extended X-ray Emissionmentioning

confidence: 99%

ChandraX-ray observations of the hyper-luminous infrared galaxy IRAS F15307+3252

Hlavacek-Larrondo

Gandhi

Hogan

et al. 2016

Mon. Not. R. Astron. Soc.

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Hyper-luminous infrared galaxies (HyLIRGs) lie at the extreme luminosity end of the IR galaxy population with L IR > 10 13 L ⊙ . They are thought to be closer counterparts of the more distant sub-mm galaxies, and should therefore be optimal targets to study the most massive systems in formation. We present deep Chandra observations of IRAS F15307+3252 (100ks), a classical HyLIRG located at z =0.93 and hosting a radio-loud AGN (L 1.4 GHz ∼ 3.5 × 10 25 W/Hz). The Chandra images reveal the presence of extended (r = 160 kpc), asymmetric X-ray emission in the soft 0.3-2.0 keV band that has no radio counterpart. We therefore argue that the emission is of thermal origin originating from a hot intragroup or intracluster medium virializing in the potential. We find that the temperature (∼ 2 keV) and bolometric X-ray luminosity (∼ 3 × 10 43 erg s −1 ) of the gas follow the expected L X−ray − T correlation for groups and clusters, and that the gas has a remarkably short cooling time of 1.2 Gyrs. In addition, VLA radio observations reveal that the galaxy hosts an unresolved compact steep-spectrum (CSS) source, most likely indicating the presence of a young radio source similar to 3C186. We also confirm that the nucleus is dominated by a redshifted 6.4 keV Fe Kα line, strongly suggesting that the AGN is Comptonthick. Finally, Hubble images reveal an over-density of galaxies and sub-structure in the galaxy that correlates with soft X-ray emission. This could be a snapshot view of on-going groupings expected in a growing cluster environment. IRAS F15307+3252 might therefore be a rare example of a group in the process of transforming into a cluster.

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“…X-ray observations of DSFGs show that the majority have bolometric luminosities that are dominated by star formation rather than AGN emission (e.g., Alexander et al 2005a;Wang et al 2013). However, these galaxies can be highly obscured by large columns of dust and gas and therefore are difficult to detect in the X-ray (e.g., Alexander et al 2005b). Radio data provide another route to distinguishing star-forming galaxies from AGN.…”

Section: Introductionmentioning

confidence: 99%

SOFIA/HAWC+ Detection of a Gravitationally Lensed Starburst Galaxy at z = 1.03

Brown

Cooray

et al. 2018

ApJ

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present the detection at 89 μm (observed frame) of the Herschel-selected gravitationally lensed starburst galaxy HATLAS J1429-0028 (also known as G15v2.19) in 15 minutes with the High-resolution Airborne Wideband Camera-plus (HAWC+) onboard the Stratospheric Observatory for Infrared Astronomy (SOFIA). The spectacular lensing system consists of an edge-on foreground disk galaxy at z=0.22 and a nearly complete Einstein ring of an intrinsic ultra-luminous infrared (IR) galaxy at z=1.03. Is this high IR luminosity powered by pure star formation (SF) or also an active galactic nucleus (AGN)? Previous nebular line diagnostics indicate that it is star formation dominated. We perform a 27-band multiwavelength spectral energy distribution (SED) modeling including the new SOFIA/HAWC+ data to constrain the fractional AGN contribution to the total IR luminosity. The AGN fraction in the IR turns out to be negligible. In addition, J1429-0028 serves as a testbed for comparing SED results from different models/templates and SED codes (MAGPHYS, SED3FIT, and CIGALE). We stress that star formation history is the dominant source of uncertainty in the derived stellar mass (as high as a factor of ∼10) even in the case of extensive photometric coverage. Furthermore, the detection of a source at z∼1 with SOFIA/HAWC+ demonstrates the potential of utilizing this facility for distant galaxy studies including the decomposition of SF/ AGN components, which cannot be accomplished with other current facilities.

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A Chandra observation of the z= 2.285 galaxy FSC 10214+4724: evidence for a Compton-thick quasar?

Cited by 26 publications

References 59 publications

Obscured and powerful AGN and starburst activities at z ~ 3.5

Obscured and powerful AGN and starburst activities at z ~ 3.5

ChandraX-ray observations of the hyper-luminous infrared galaxy IRAS F15307+3252

SOFIA/HAWC+ Detection of a Gravitationally Lensed Starburst Galaxy at z = 1.03

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