The properties and environment of the giant, infrared-luminous galaxy IRAS 09104 + 4109

Kleinmann, S. G.; Hamilton, D.; Keel, William C.; Wynn‐Williams, C. G.; Eales, Stephen Anthony; Becklin, E. E.; Küntz, K. D.

doi:10.1086/166276

Cited by 101 publications

(118 citation statements)

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“…About 30% are in the hyperluminous class (L IR > 10 13 L ; Kleinmann et al 1988; see also Rowan-Robinson 2000), 41% are ULIRGs (L IR ¼ 10 12 10 13 L ), and all but one of the rest are LIRGs (L IR ¼ 10 11 10 12 L ). Figure 5 shows the distribution of IR luminosities.…”

Section: Rest-frame 12 M and Total Ir Luminositiesmentioning

confidence: 99%

Infrared Power‐Law Galaxies in the Chandra Deep Field–South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies

Alonso‐Herrero

Pérez‐González

Alexander

et al. 2006

ApJ

239

308

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We investigate the nature of a sample of 92 Spitzer MIPS 24 m-selected galaxies in the CDF-S, showing powerlaw-like emission in the Spitzer IRAC 3.6-8 m bands. The main goal is to determine whether the galaxies not detected in X-rays (47% of the sample) are part of the hypothetical population of obscured AGNs not detected even in deep X-ray surveys. The majority of the IR power-law galaxies are ULIRGs at z > 1, and those with LIRG-like IR luminosities are usually detected in X-rays. The optical-to-IR SEDs of the X-ray-detected galaxies are almost equally divided between a BLAGN SED class (similar to an optically selected QSO) and an NLAGN SED (similar to the BLAGN SED but with an obscured UV/optical continuum). A small fraction of SEDs resemble warm ULIRGs (e.g., Mrk 231). Most galaxies not detected in X-rays have SEDs in the NLAGN+ULIRG class as they tend to be optically fainter and possibly more obscured. Moreover, the IR power-law galaxies have SEDs significantly different from those of high-z (z sp > 1) IR (24 m) selected and optically bright ( VVDS I AB 24) star-forming galaxies whose SEDs show a very prominent stellar bump at 1.6 m. The galaxies detected in X-rays have 2-8 keV rest-frame luminosities typical of AGNs. The galaxies not detected in X-rays have global X-ray-to-mid-IR SED properties that make them good candidates to contain IR-bright X-ray-absorbed AGNs. If all these sources are actually obscured AGNs, we would observe a ratio of obscured to unobscured 24 m-detected AGNs of 2:1, whereas models predict a ratio of up to 3:1. Additional studies using Spitzer to detect X-ray-quiet AGNs are likely to find more such obscured sources.

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Section: Rest-frame 12 M and Total Ir Luminositiesmentioning

confidence: 99%

Infrared Power‐Law Galaxies in the Chandra Deep Field–South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies

Alonso‐Herrero

Pérez‐González

Alexander

et al. 2006

ApJ

239

308

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“…Its optical spectrum is that of an Sy2 (Kleinmann et al 1988;Soifer et al 1996;Véron-Cetty & Véron 2006), but with broad Hβ, Hγ, and Mg II lines in polarized light (Hines & Wills 1993;Tran et al 2000). There is also a polarized, bipolar reflection nebula centered on the nucleus (Hines et al 1999).…”

Section: Introductionmentioning

confidence: 99%

“…IRAS 09104+4109 (Kleinmann et al 1988) at z = 0.442 (Hewett & Wild 2010) is one such archetype, for the relationship between luminous, obscured AGNs and star formation. In the radio it is a "radio-intermediate" FR-I source, with a linear core and double-lobed structure (Hines & Wills 1993;O'Sullivan et al 2012).…”

Section: Introductionmentioning

confidence: 99%

The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar

Farrah

Baloković

Stern

et al. 2016

ApJ

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We study the geometry of the active galactic nucleus (AGN) obscurer in IRAS 09104+4109, an IR-luminous, radio-intermediate FR-I source at z = 0.442, using infrared data from Spitzer and Herschel, X-ray data from NuSTAR, Swift, Suzaku, and Chandra, and an optical spectrum from Palomar. The infrared data imply a total restframe 1-1000 μm luminosity of 5.5×10 46 erg s −1 and require both an AGN torus and a starburst model. The AGN torus has an anisotropy-corrected IR luminosity of 4.9×10 46 erg s −1 and a viewing angle and half-opening angle both of approximately 36°from pole-on. The starburst has a star formation rate of (110±34) M e yr −1 and an age of <50 Myr. These results are consistent with two epochs of luminous activity in IRAS 09104+4109: one approximately 150 Myr ago, and one ongoing. The X-ray data suggest a photon index of Γ ; 1.8 and a line-ofsight column density of N H ; 5×10 23 cm −2 . This argues against a reflection-dominated hard X-ray spectrum, which would have implied a much higher N H and luminosity. The X-ray and infrared data are consistent with a bolometric AGN luminosity of L bol ∼(0.5-2.5)×10 47 erg s −1. The X-ray and infrared data are further consistent with coaligned AGN obscurers in which the line of sight "skims" the torus. This is also consistent with the optical spectra, which show both coronal iron lines and broad lines in polarized but not direct light. Combining constraints from the X-ray, optical, and infrared data suggestthat the AGN obscurer is within a vertical height of 20 pc, and a radius of 125 pc, of the nucleus.

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“…BeppoSAX detected a hard X-ray excess (Franceschini et al 2000) above the previously known cluster emission around IRAS 09104+4109, one of the hyperluminous infrared galaxies at z = 0.442 (Kleinmann et al 1988). A follow-up Chandra observation clearly detected a reflection-dominated X-ray nucleus, spatially separated from the surrounding cluster emission (Iwasawa, Fabian & Ettori 2001).…”

Section: Obscured a G N At High Redshiftmentioning

confidence: 75%

The Obscured AGN Population Probed by X-ray Observations

Iwasawa

2002

International Astronomical Union Colloquium

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Abstract. X-ray properties of obscured AGN are reviewd and recent results obtained from ASCA, BeppoSAX, and Chandra are presented.There is a population of AGN that can only be revealed by hard X-ray observations. Studies of the X-ray background suggest that obscured AGN should significantly outnumber their unobscured counterparts. X-ray Spectra of Obscured AGN Effects of X-ray AbsorptionThe energy distribution of AGN can be approximated by a power-law and is roughly fiat over the X-ray band. However, we now know at least in wellstudied bright Seyfert galaxies that there are a significant excess of soft X-ray (below half keV) emission and a roll-over of the hard X-ray continuum at a few hundred keV. The soft X-ray excess is believed to be related to the accretion disk while the high energy roll-over is probably due to a cut-off in energy of thermal electrons in a corona which Comptonizes the disk emission into the power-law continuum. There are other subtle spectral distortions due to reflection off the accretion disk surface. These phenomena are likely happening in a region within 100 gravitational radii of a central black hole.When cold matter lies in the line of sight at radii much further out, a series of photoelectric edges of various elements as well as Hydrogen are imposed on the X-ray continuum and make a low energy cut-off. The energy of the absorption cut-off increases as the column density of the absorbing matter increases. Therefore, going up across the X-ray energy band has the same effect as increasing wavelength in the optical/near-infrared for obscured objects. Assuming the Galactic dust to gas ratio, the optical depth which a near-infrared observation (say, in the K band) can probe is equivalent to that at 2-3 keV. For example, ROSAT, whose bandpass was up to 2 keV, was sensitive to relatively unobscured AGN but no longer sensitive when an absorption column density exceeds 10 22 cm -2 (of course, this restriction is relaxed for high redshift objects). X-ray observatories such as ASCA, BeppoSAX, Chandra and XMMNewton have sensitivity above 2 keV, which enables these satellites to search for highly obscured AGN. It should, however, be noted that simply shifting the energy window to higher energies does not necessarily guarantee detection of more heavily obscured objects, because of a) increasing importance of Comp- 225terms of use, available at https://www.cambridge.org/core/terms. https://doi

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The properties and environment of the giant, infrared-luminous galaxy IRAS 09104 + 4109

Cited by 101 publications

References 0 publications

Infrared Power‐Law Galaxies in the Chandra Deep Field–South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies

Infrared Power‐Law Galaxies in the Chandra Deep Field–South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies

The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar

The Obscured AGN Population Probed by X-ray Observations

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