Warm ultraluminous galaxies in the IRAS survey - The transition from galaxy to quasar?

Sanders, D. B.; Soifer, B. T.; Elias, J. H.; Neugebauer, G.; Matthews, K.

doi:10.1086/185155

Cited by 540 publications

(549 citation statements)

References 4 publications

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“…These broad lines are generally seen at longer wavelengths (i.e., Hα and possibly Hβ), which sufferless from dust extinction and host-galaxy dilution, and may be reddened Type 1.8 and 1.9 AGNs, 21 rather than pure Type 1 AGNs, since higher-ionization lines such as Mg II are narrow or absent (e.g., Brusa et al 2015). These reddened AGNs are an interesting class of objects, and at least some appear to be in a transition stage between an obscured and unobscured phase within the merger-induced galaxy/black hole co-evolution paradigm (Sanders et al 1988;Hopkins et al 2005;Brusa et al 2010;Banerji et al 2012;Farrah et al 2012;Glikman et al 2012). Indeed, the Hubble Space Telescope followedup a handful of these objects and revealed that they live in trainwreck host galaxies, indicative of merger activity (Urrutia et al 2008;Glikman et al 2015).…”

Section: Selecting Reddened Broad-lined Agnsmentioning

confidence: 99%

On R − W1 as a Diagnostic to Discover Obscured Active Galactic Nuclei in Wide-Area X-Ray Surveys

LaMassa

Civano

Brusa

et al. 2016

ApJ

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Capitalizing on the all-sky coverage of WISEand the 35% and 50% sky coverage from Sloan Digital Sky Survey and Pan-STARRS, respectively, we explore the efficacy of-, as a color diagnostic to identify obscured supermassive black hole accretion in wide-area X-ray surveys. We use the ∼16.5 deg 2 Stripe 82 X-ray survey data as a testbed to compare R W1 -with R−K, an oft-used obscured active galactic nucleus (AGN) selection criterion, and examine where different classes of objects lie in this parameter space. Most stars follow a well-defined path in R−K versus R W1space. We demonstrate that optically normal galaxies hosting X-ray AGNs at redshifts z 0.5 1 < < can be recovered with an R W1 4 -> colorcut, while they typically are not selected as AGNs based on their W W 1 2 -colors. Additionally, different observed X-ray luminosity bins favor different regions in R W1 -parameter space: moderate-luminosity AGNs > -erg s −1 ) have bluer colors; higher spectroscopic completeness of the Stripe 82X sample is needed to determine whether this is a selection effect or an intrinsic property. Finally, we parameterize X-ray obscuration of Stripe 82X AGNs by calculating their hardness ratios (HRs) and find no clear trends between HR and optical reddening. Our results will help inform best-effort practices in followingup obscured AGN candidates in current and future wide-area, shallow X-ray surveys, including the all-sky eROSITA mission.

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Section: Selecting Reddened Broad-lined Agnsmentioning

confidence: 99%

On R − W1 as a Diagnostic to Discover Obscured Active Galactic Nuclei in Wide-Area X-Ray Surveys

LaMassa

Civano

Brusa

et al. 2016

ApJ

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“…One direct way to test the model presented by Sanders et al (1988b) observationally is to probe this evolutionary sequence at the 'transition stage' where the youthful QSOs are just beginning to shed their cocoons of gas and dust (e.g. Coppin et al 2008;Simpson et al 2012).…”

Section: Introductionmentioning

confidence: 99%

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Violino¹,

Coppin²,

Stevens³

et al. 2016

Mon. Not. R. Astron. Soc.

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It is thought that a class of broad absorption line (BAL) QSOs, characterised by Fe absorption features in their UV spectra (called 'FeLoBALs'), could mark a transition stage between the end of an obscured starburst event and a youthful QSO beginning to shed its dust cocoon, where Fe has been injected into the interstellar medium by the starburst. To test this hypothesis we have undertaken deep SCUBA-2 850 µm observations of a sample of 17 FeLoBAL QSOs with 0.89 z 2.78 and -23.31 M B -28.50 to directly detect an excess in the thermal emission of the dust which would probe enhanced star-formation activity. We find that FeLoBALs are not luminous sources in the submillimetre, none of them are individually detected at 850 µm, nor as a population through stacking (F s = 1.14 ± 0.58 mJy). Statistical and survival analyses reveal that FeLoBALs have sub-mm properties consistent with BAL and non-BAL QSOs with matched redshifts and magnitudes. An SED fitting analysis shows that the FIR emission is dominated by AGN activity, and a starburst component is required only in 6/17 sources of our sample; moreover the integrated total luminosity of 16/17 sources is L 10 12 L , high enough to classify FeLoBALs as infrared luminous.In conclusion, we do not find any evidence in support of FeLoBAL QSOs being a transition population between a ULIRG and an unobscured QSO; in particular, FeLoBALs are not characterized by a cold starburst which would support this hypothesis.

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“…Ultraluminous infrared galaxies (ULIRGs) have been found to be ubiquitously strong, interacting merger systems heated by star-forming and/or AGN power sources (e.g., Genzel et al 1998). They have been hypothesized to evolve into normal quasars after the central engine clears away the dust associated with the massive burst of star formation (Sanders et al 1988;Sanders & Mirabel 1996;Veilleux 2006). These objects are possibly the first observational snapshot in merger evolution and formation of a larger elliptical galaxy.…”

Section: Introductionmentioning

confidence: 99%

Post-starburst quasars: bridging the gap between post-starburst galaxies and quasars

Cales

Brotherton

2015

Monthly Notices of the Royal Astronomical Society

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In order to better understand the nature of post-starburst quasars (PSQs) in the context of galaxy evolution, we compare their properties to those of post-starburst galaxies and quasars from appropriately selected samples possessing similar redshift (z ∼ 0.3), luminosity (M r ∼ −23), and data quality. We consider morphologies, spectral features, and derived physical properties of the stellar populations and central supermassive black hole. PSQs themselves come in two types: the more luminous AGNs with more luminous post-starburst stellar populations hosted by elliptical galaxies, some which are clearly merger products, and the less luminous systems existing within relatively undisturbed spiral galaxies and possessing signs of a more extended period of star formation. Post-starburst galaxies (PSQs) have elliptical and disturbed/postmerger morphologies similar to those of the more luminous PSQs, display similar spectral properties, but also can have younger stellar populations for a given starburst mass. Quasars at similar redshifts and luminosities around the Seyfert/quasar transition possess similar AGN characteristics, in terms of black hole mass and accretion rate, compared with those of PSQs, but do not appear to be hosted by galaxies with significant post-starburst populations. Recent studies of more luminous quasars find hosts consistent with those of our luminous PSQs, suggesting that these PSQs may be in transition between post-starburst galaxies and a more luminous quasar stage when the post-starburst stellar population remains dominant. The lower luminosity PSQs appear to differ from lower luminosity quasars (Seyfert galaxies) in terms of more significant star formation in their past.

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Warm ultraluminous galaxies in the IRAS survey - The transition from galaxy to quasar?

Cited by 540 publications

References 4 publications

On R − W1 as a Diagnostic to Discover Obscured Active Galactic Nuclei in Wide-Area X-Ray Surveys

On R − W1 as a Diagnostic to Discover Obscured Active Galactic Nuclei in Wide-Area X-Ray Surveys

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Post-starburst quasars: bridging the gap between post-starburst galaxies and quasars

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