Iras F13308+5946: A Possible Transition Phase From Type I Ultraluminous Infrared Galaxy to Optical Quasar

Meng, Xia; Wu, Hong; Gu, Qing; Wang, Jing; Cao, Chen

doi:10.1088/0004-637x/718/2/928

Cited by 12 publications

(17 citation statements)

References 89 publications

(124 reference statements)

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“…This selection of templates is widely used in the literature and has shown to provide reasonable results to similar classes of sources over the NIR-to-mm wavelength regime (i.e. Efstathiou, Rowan-Robinson & Siebenmorgen 2000;Siebenmorgen et al 2004;Meng et al 2010;Serra et al 2011;Younger & Hopkins 2011;Yun et al 2012, and references therein). For this work, we favor the Siebenmorgen et al (2004) AGN models as opposed to torus models as we are more interested in the integrated AGN host properties rather than the centralized nuclear region.…”

Section: Nir-to-radio Sed Modelingmentioning

confidence: 99%

X-ray detections of submillimetre galaxies: active galactic nuclei versus starburst contribution

Johnson¹,

Wilson²,

Wang³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We present a large-scale study of the X-ray properties and near-IR-to-radio spectral energy distributions (SEDs) of submillimetre galaxies (SMGs) detected at 1.1mm with the AzTEC instrument across a ∼1.2 square degree area of the sky. Combining deep 2 − 4 Ms Chandra data with Spitzer IRAC/MIPS and VLA data within the GOODS-N, GOODS-S and COSMOS fields, we find evidence for AGN activity in ∼14 percent of 271 AzTEC SMGs, ∼28 percent considering only the two GOODS fields. Through X-ray spectral modeling and multi-wavelength SED fitting using Monte Carlo Markov Chain techniques to Siebenmorgen et al. (2004) (AGN) and Efstathiou, Rowan-Robinson & Siebenmorgen (2000) (starburst) templates, we find that while star formation dominates the IR emission, with star formation rates (SFRs) ∼ 100 − 1000 M ⊙ yr −1 , the X-ray emission for most sources is almost exclusively from obscured AGNs, with column densities in excess of 10 23 cm −2 . Only for ∼6 percent of our sources do we find an X-ray-derived SFR consistent with NIR-to-radio SED derived SFRs. Inclusion of the X-ray luminosities as a prior to the NIR-to-radio SED effectively sets the AGN luminosity and SFR, preventing significant contribution from the AGN template. Our SED modeling further shows that the AGN and starburst templates typically lack the required 1.1 mm emission necessary to match observations, arguing for an extended, cool dust component. The cross correlation function between the full samples of X-ray sources and SMGs in these fields does not indicate a strong correlation between the two populations at large scales, suggesting that SMGs and AGNs do not necessarily trace the same underlying large scale structure. Combined with the remaining X-ray-dim SMGs, this suggests that sub-mm bright sources may evolve along multiple tracks, with X-ray-detected SMGs representing transitionary objects between periods of high star formation and AGN activity while X-ray-faint SMGs represent a brief starburst phase of more normal galaxies.

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Section: Nir-to-radio Sed Modelingmentioning

confidence: 99%

X-ray detections of submillimetre galaxies: active galactic nuclei versus starburst contribution

Johnson¹,

Wilson²,

Wang³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…The spectral synthesis code STARLIGHT (Cid Fernandes et al 2005) is used to derive the stellar populations of different star formation regions along the bar. Previous studies have shown that this spectrum fitting code is a good tool for studying the properties of various types of galaxies (e.g., Meng et al 2010;Lara-López et al 2010;Martins et al 2010). Our template spectra consist of simple stellar populations (SSPs) from Bruzual & Charlot (2003).…”

Section: Stellar Populationmentioning

confidence: 99%

Star Formation Properties in Barred Galaxies (Sfb). I. Ultraviolet to Infrared Imaging and Spectroscopic Studies of NGC 7479

Zhang

Cao

Meng

et al. 2011

The Astronomical Journal

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Large-scale bars and minor mergers are important drivers for the secular evolution of galaxies. Based on ground-based optical images and spectra as well as ultraviolet data from the Galaxy Evolution Explorer and infrared data from the Spitzer Space Telescope, we present a multi-wavelength study of star formation properties in the barred galaxy NGC 7479, which also has obvious features of a minor merger. Using various tracers of star formation, we find that under the effects of both a stellar bar and a minor merger, star formation activity mainly takes place along the galactic bar and arms, while the star formation rate changes from the bar to the disk. With the help of spectral synthesis, we find that strong star formation took place in the bar region about 100 Myr ago, and the stellar bar might have been ∼10 Gyr old. By comparing our results with the secular evolutionary scenario from Jogee et al., we suggest that NGC 7479 is possibly in a transitional stage of secular evolution at present, and it may eventually become an earlier type galaxy or a luminous infrared galaxy. We also note that the probable minor merger event happened recently in NGC 7479, and we find two candidates for minor merger remnants.

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“…The AGN in ULIRGs may become more important with increasing IR luminosity, and advancing merger stage (Teng & Veilleux 2010;Yuan et al 2010;Stierwalt et al 2013), and sometimes initiate powerful outflows (Spoon et al 2009;Fischer et al 2010;Rupke & Veilleux 2011;Sturm et al 2011;Westmoquette et al 2012;Rodríguez Zaurín et al 2013). A small fraction of (low-redshift) ULIRGs become optical QSOs (Tacconi et al 2002;Kawakatu et al 2006Kawakatu et al , 2007Farrah et al 2007b;Meng et al 2010;Hou et al 2011) and a large fraction end up as early-type galaxies (Genzel et al 2001;Dasyra et al 2006;Rothberg et al 2013;Wang et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Far-Infrared Fine-Structure Line Diagnostics of Ultraluminous Infrared Galaxies

Farrah

Lebouteiller

Spoon

et al. 2013

ApJ

161

213

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We present Herschel observations of six fine-structure lines in 25 Ultraluminous Infrared Galaxies at z < 0.27. The lines, [O III]52µm, [N III]57µm, [O I]63µm, [N II]122µm, [O I]145µm, and [C II]158µm, are mostly single gaussians with widths <600 km s −1 and luminosities of 10 7 − 10 9 L ⊙ . There are deficits in the [O I]63/L IR , [N II]/L IR , [O I]145/L IR , and [C II]/L IR ratios compared to lower luminosity systems. The majority of the line deficits are consistent with dustier H II regions, but part of the [C II] deficit may arise from an additional mechanism, plausibly charged dust grains. This is consistent with some of the [C II] originating from PDRs or the ISM. We derive relations between far-IR line luminosities and both IR luminosity and star formation rate. We find that [N II] and both [O I] lines are good tracers of IR luminosity and star formation rate. In contrast, [C II] is a poor tracer of IR luminosity and star formation rate, and does not improve as a tracer of either quantity if the [C II] deficit is accounted for. The continuum luminosity densities also correlate with IR luminosity and star formation rate. We derive ranges for the gas density and ultraviolet radiation intensity of 10 1 < n < 10 2.5 and 10 2.2 < G 0 < 10 3.6 , respectively. These ranges depend on optical type, the importance of star formation, and merger stage. We do not find relationships between far-IR line properties and several other parameters; AGN activity, merger stage, mid-IR excitation, and SMBH mass. We conclude that these far-IR lines arise from gas heated by starlight, and that they are not strongly influenced by AGN activity.

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Iras F13308+5946: A Possible Transition Phase From Type I Ultraluminous Infrared Galaxy to Optical Quasar

Cited by 12 publications

References 89 publications

X-ray detections of submillimetre galaxies: active galactic nuclei versus starburst contribution

X-ray detections of submillimetre galaxies: active galactic nuclei versus starburst contribution

Star Formation Properties in Barred Galaxies (Sfb). I. Ultraviolet to Infrared Imaging and Spectroscopic Studies of NGC 7479

Far-Infrared Fine-Structure Line Diagnostics of Ultraluminous Infrared Galaxies

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