On the nature of the absorber in IRAS 09104+4109: the X-ray and mid-infrared view

Vignali, C.; Piconcelli, E.; Lanzuisi, G.; Feltre, Anna; Feruglio, C.; Maiolino, R.; Fiore, F.; Fritz, J.; Parola, V. La; Mignoli, M.; Pozzi, F.

doi:10.1111/j.1365-2966.2011.19181.x

Cited by 30 publications

(52 citation statements)

References 87 publications

(125 reference statements)

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“…This result and the heavy X-ray absorption shown by most of these sources (all but one source, IRAS 14026+4341, show signatures of CT absorption in their X-ray emission, see Wilman et al 2003;Iwasawa et al 2005;Ruiz et al 2007Ruiz et al , 2010Vignali et al 2011) point towards large amounts of gas and dust enshrouding their nuclear environment as found in local ULIRG (Spoon et al 2004b;Verma et al 2005;Yan et al 2010).…”

Section: Covering Factormentioning

confidence: 71%

Analysis ofSpitzer-IRS spectra of hyperluminous infrared galaxies

Ruiz¹,

Risaliti²,

Nardini³

et al. 2013

A&A

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Context. Hyperluminous infrared galaxies (HLIRG) are the most luminous persistent objects in the Universe. They exhibit extremely high star formation rates, and most of them seem to harbour an active galactic nucleus (AGN). They are unique laboratories for investigating the most extreme star formation and its connection to super-massive black hole growth. Aims. The relative AGN and starburst (SB) contributions to the total output in these objects is still debated. Our aim is to disentangle the AGN and SB emission of a sample of thirteen HLIRG. Methods. We studied the MIR low-resolution spectra of a sample of thirteen HLIRG obtained with the Infrared Spectrograph on board Spitzer. The 5−8 µm range is an optimal window for detecting AGN activity even in a heavily obscured environment. We performed an SB/AGN decomposition of the continuum using templates, which has been successfully applied for ULIRG in previous works. Results. The MIR spectra of all sources is largely dominated by AGN emission. By converting the 6 µm luminosity into IR luminosity, we found that ∼80% of the sample shows an IR output dominated by the AGN emission. However, the SB activity is significant in all sources (mean SB contribution ∼30%), showing star formation rates ∼300−3000 M yr −1 . With X-ray and MIR data we estimated the dust covering factor (CF) of these HLIRG, finding that a significant fraction presents a CF consistent with unity. Along with the high X-ray absorption shown by these sources, this suggests that large amounts of dust and gas enshroud the nucleus of these HLIRG, as also observed in ULIRG. Conclusions. Our results agree with previous studies of the IR SED of HLIRG using radiative transfer models, and we find strong evidence that all HLIRG harbour an AGN. Moreover, this work provides further support for the idea that AGN and SB are both crucial to understanding the properties of HLIRG. Our study of the CF supports the hypothesis that HLIRG can be divided into two different populations.

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Section: Covering Factormentioning

confidence: 71%

Analysis ofSpitzer-IRS spectra of hyperluminous infrared galaxies

Ruiz¹,

Risaliti²,

Nardini³

et al. 2013

A&A

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“…The source is detected from the observed mid-IR bands (where both Spitzer warm-mission data and AllWISE data are available) to the sub-mm band (SCUBA-2). This broadband coverage allows us to provide a good modeling of the SED in terms of an AGN plus a starburst component using the fitting code originally developed by Fritz et al (2006), recently updated by Feltre et al (2012), see Vignali et al (2011) Fig. 3.…”

Section: Sed Of W1835+4355mentioning

confidence: 99%

The hidden quasar nucleus of a WISE-selected, hyperluminous, dust-obscured galaxy atz~ 2.3

Piconcelli

Vignali

Bianchi

et al. 2015

A&A

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We present the first X-ray spectrum of a hot dust-obscured galaxy (DOG), namely W1835+4355 at z ∼ 2.3. Hot DOGs represent a very rare population of hyperluminous (≥10 47 erg s −1 ), dust-enshrouded objects at z ≥ 2 recently discovered in the WISE All Sky Survey. The 40 ks XMM-Newton spectrum reveals a continuum as flat (Γ ∼ 0.8) as typically seen in heavily obscured AGN. This, along with the presence of strong Fe Kα emission, clearly suggests a reflection-dominated spectrum due to Compton-thick absorption. In this scenario, the observed luminosity of L 2−10 ∼ 2 × 10 44 erg s −1 is a fraction (<10%) of the intrinsic one, which is estimated to be > ∼ 5 × 10 45 erg s −1 by using several proxies. The Herschel data allow us to constrain the SED up to the sub-mm band, providing a reliable estimate of the quasar contribution (∼75%) to the IR luminosity as well as the amount of star formation (∼2100 M yr −1 ). Our results thus provide additional pieces of evidence that associate Hot DOGs with an exceptionally dusty phase during which luminous quasars and massive galaxies co-evolve and a very efficient and powerful AGN-driven feedback mechanism is predicted by models.

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“…This component is extincted according to a Calzetti et al (2000) attenuation law. For the AGN component, we used an extended grid of "smooth" torus models with a "flared disc" geometry (Fritz et al 2006), which provides a good description of the AGN mid-IR SED in the case of sparse photometric datapoints (see also Vignali et al 2011;and Feltre et al 2012).…”

Section: Spectral Energy Distribution Of Pid352mentioning

confidence: 99%

“…Using the bolometric luminosity of PID352 (∼10 46 erg s −1 ) derived from the SED fitting and ascribed to accretion processes (i.e., the mid-IR emission as due to thermally reprocessed AGN emission; see Vignali et al 2011, for details) and assuming an energy conversion factor η = 0.1, we obtain acc ≈ 1.7 M yr −1 , i.e., of the same order of magnitude as the mass outflow rate.…”

Section: Radio Datamentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

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In active galactic nuclei (AGN)-galaxy co-evolution models, AGN winds and outflows are often invoked to explain why super-massive black holes and galaxies stop growing efficiently at a certain phase of their lives. They are commonly referred to as the leading actors of feedback processes. Evidence of ultra-fast (v > ∼ 0.05c) outflows in the innermost regions of AGN has been collected in the past decade by sensitive X-ray observations for sizable samples of AGN, mostly at low redshift. Here we present ultra-deep XMM-Newton and Chandra spectral data of an obscured (N H ≈ 2 × 10 23 cm −2 ), intrinsically luminous (L 2−10 keV ≈ 4 × 10 44 erg s −1 ) quasar (named PID352) at z ≈ 1.6 (derived from the X-ray spectral analysis) in the Chandra Deep Field-South. The source is characterized by an iron emission and absorption line complex at observed energies of E ≈ 2−3 keV. While the emission line is interpreted as being due to neutral iron (consistent with the presence of cold absorption), the absorption feature is due to highly ionized iron transitions (FeXXV, FeXXVI) with an outflowing velocity of 0.14 +0.02 −0.06 c, as derived from photoionization models. The mass outflow rate -∼2 M yr −1 -is similar to the source accretion rate, and the derived mechanical energy rate is ∼9.5 × 10 44 erg s −1 , corresponding to 9% of the source bolometric luminosity. PID352 represents one of the few cases where indications of X-ray outflowing gas have been observed at high redshift thus far. This wind is powerful enough to provide feedback on the host galaxy.

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On the nature of the absorber in IRAS 09104+4109: the X-ray and mid-infrared view

Cited by 30 publications

References 87 publications

Analysis ofSpitzer-IRS spectra of hyperluminous infrared galaxies

Analysis ofSpitzer-IRS spectra of hyperluminous infrared galaxies

The hidden quasar nucleus of a WISE-selected, hyperluminous, dust-obscured galaxy atz~ 2.3

The XMM deep survey in the CDF-S

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