Statistical Properties of Ultraluminous [ITAL]IRAS[/ITAL] Galaxies from an [ITAL]HST[/ITAL] Imaging Survey

Cui, Jun; Xia, X. Y.; Deng, Z. G.; Mao, Shude; Zou, Zhimin

doi:10.1086/321127

Cited by 52 publications

(62 citation statements)

References 61 publications

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“…It has been shown to have a single nucleus based upon HST observations (Cui et al 2001). The infrared luminosity that we measure (Table 4.2) is consistent with previous measurements (Cui et al 2001) and our AGN luminosity measurement is consistent with that derived from Spitzer infrared spectroscopy (Sargsyan et al 2008).…”

Section: J0945+1737supporting

confidence: 91%

Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies

Harrison¹

2016

Springer Theses

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How to cite: HARRISON, CHRISTOPHER,MARK (2014) Observational constraints on the inuence of active galactic nuclei on the evolution of galaxies, Durham The 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 Durham E-Theses• the full-text is not changed in any wayThe full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full Durham E-Theses policy for further details. Observational constraints on the influence of active galactic nuclei on the evolution of galaxies Christopher Mark Harrison AbstractAt the centre of every massive galaxy there resides a super-massive black hole that grew during periods of active galactic nuclei (AGN) activity. Current theoretical models of galaxy evolution invoke AGN-driven galaxy-scale feedback processes (e.g., the expulsion of gas through outflows) in order to reproduce many of the fundamental properties of galaxies and the intergalactic medium. This thesis uses observations to test some of the predictions of these feedback processes. I present integral field unit observations of AGN host galaxies to trace their ionised gas kinematics. The targets are eight high-redshift (z = 1.4 −3.4) ultra-luminous infrared galaxies, that are representative of rapidly evolving distant galaxies, and sixteen z < 0.2 luminous AGN, that were selected from a parent sample of ≈24,000 sources to be representative of the overall population. In both samples I identify galaxy-wide outflows (i.e., over kiloparsec scales), calculate their properties (e.g., mass outflow rates and energetics) and show that they are broadly consistent with theoretical predictions. I find that ionised outflows are common in z < 0.2 luminous AGN and are consistently extended over kiloparsec scales (in ≥ 70% of cases). I also use far-infrared Herschel data of X-ray detected z = 1-3 AGN to test the prediction that luminous AGN shut down star formation in their host galaxies. Using stacking techniques I show that, on average, X-ray detected AGN over a wide range of luminosities (i.e., L 2−8keV ≈ 10 42−45 erg s −1 ) have star formation rates that are consistent with non-active galaxies. This may imply that luminous AGN do not impact upon the star formation in their host galaxies. Overall, this thesis demonstrates that energetic galaxy-wide outflows are prevalent in AGN host galaxies; however, it also demonstrates that we still lack direct observational evidence that luminous AGN are suppressing star formation in their host galaxies.

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Section: J0945+1737supporting

confidence: 91%

Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies

Harrison¹

2016

Springer Theses

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“…• IRAS 21130-4446: This ULIRG is identified as a double nucleus system with a nuclear separation ∼5 kpc, however, the complex morphology of the galaxy makes it hard to locate the exact position of the two nuclei (Cui et al 2001). The WFPC2 F814W image of this source shows different condensations and tails, some of them unresolved in our SINFONI data, which cover ∼14 × 14 kpc centred in the northern nucleus of the galaxy.…”

Section: Stellar Componentmentioning

confidence: 94%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2012

A&A

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We present an atlas of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7) covering the luminosity range log(L IR /L ) = 11.1−12.4. The atlas is based on near-infrared H (1.45−1.85 μm) and K-band (1.95−2.45 μm) VLT-SINFONI integral field spectroscopy (IFS). The atlas presents the ionised, partially ionised, and warm molecular gas two-dimensional flux distributions and kinematics over an FoV of ∼3 × 3 kpc (LIRGs) and ∼12 × 12 kpc (ULIRGs) and with average linear resolutions of ∼0.2 kpc and ∼0.9 kpc, respectively. The different phases of the gas show a wide morphological variety with the nucleus as the brightest Brγ source for ∼33% of the LIRGs and ∼71% of the ULIRGs, whereas all the LIRGs and ULIRGs have their maximum H 2 emission in their nuclear regions. In LIRGs, the ionised gas distribution is dominated by the emission from the star-forming rings or giant HII regions in the spiral arms. The Brγ and [FeII] line at 1.644 μm trace the same structures, although the emission peaks at different locations in some of the objects, and the [FeII] seems to be more extended and diffuse. The ULIRG subsample is at larger distances and contains mainly pre-coalescence interacting systems. Although the peaks of the molecular gas emission and the continuum coincide in ∼71% of the ULIRGs, regions with intense Paα (Brγ) emission tracing luminous star-forming regions located at distances of 2−4 kpc away from the nucleus are also detected, usually associated with secondary nuclei or tidal tails. LIRGs have mean observed (i.e. uncorrected for internal extinction) SFR surface densities of about 0.4 to 0.9 M yr −1 kpc −2 over large areas (4−9 kpc 2 ) with peaks of about 2−2.5 M yr −1 kpc −2 in the smaller regions (0.16 kpc 2 ) associated with the nucleus of the galaxy or the brightest Brγ region. ULIRGs do have similar average SFR surface densities for the integrated emitting regions of ∼0.4 M yr −1 kpc −2 in somewhat larger areas (100−200 kpc 2 ) and for the Paα peak (∼2 M yr −1 kpc −2 in 4 kpc 2 ). The observed gas kinematics in LIRGs is primarily due to rotational motions around the centre of the galaxy, although local deviations associated with radial flows and/or regions of higher velocity dispersions are present. The ionised and molecular gas share the same kinematics (velocity field and velocity dispersion) to first order, showing slight differences in the velocity amplitudes (peak-to-peak) in some cases, whereas the average velocity dispersions are compatible within uncertainties. As expected, the kinematics of the ULIRG subsample is more complex, owing to the interacting nature of the objects of the sample.

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“…Arribas et al 2004;Alonso-Herrero et al 2006;Sanders & Ishida 2004), most of the ULIRGs show signs of a clear merging process (e.g. Clements et al 1996;Borne et al 2000;Cui et al 2001;Bushouse et al 2002;Veilleux et al 2002). While (U)LIRGs are an oddity in the local Universe, recent midinfrared and submillimeter surveys show how they present a strong evolution with redshift, increasing their number by two orders of magnitude at z ∼ 0.8−1.2 (Elbaz et al 2002).…”

Section: Introductionmentioning

confidence: 99%

VLT-VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies

Monreal-Ibero

Arribas

Colina

et al. 2010

A&A

101

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Context. Luminous infrared galaxies (LIRGs) are an important class of objects in the low-z universe bridging the gap between normal spirals and the strongly interacting and starbursting ultraluminous infrared galaxies (ULIRGs). Since a large fraction of the stars in the Universe have been formed in these objects, LIRGs are also relevant in a high-z context. Studies of the two-dimensional physical properties of LIRGs are still lacking. Aims. We aim to understand the nature and origin of the ionization mechanisms operating in the extra-nuclear regions of LIRGs as a function of the interaction phase and infrared luminosity. Methods. This study uses optical integral field spectroscopy (IFS) data obtained with VIMOS. Our analysis is based on over 25 300 spectra of 32 LIRGs covering all types of morphologies (isolated galaxies, interacting pairs, and advanced mergers), and the entire 10 11 −10 12 L infrared luminosity range. Results. We found strong evidence for shock ionization, with a clear trend with the dynamical status of the system. Specifically, we quantified the variation with interaction phase of several line ratios indicative of the excitation degree. While the [N ii]λ6584/Hα ratio does not show any significant change, the [S ii]λλ6717,6731/Hα and [O i]λ6300/Hα ratios are higher for more advanced interaction stages. Velocity dispersions are higher than in normal spirals and increase with the interaction class (medians of 37, 46, and 51 km s −1 for class 0−2, respectively). We constrained the main mechanisms causing the ionization in the extra-nuclear regions (typically for distances ranging from ∼0.2−2.1 kpc to ∼0.9−13.2 kpc) using diagnostic diagrams. Isolated systems are mainly consistent with ionization caused by young stars. Large fractions of the extra-nuclear regions in interacting pairs and more advanced mergers are consistent with ionization caused by shocks of v s < ∼ 200 km s −1 . This is supported by the relation between the excitation degree and the velocity dispersion of the ionized gas, which we interpret as evidence for shock ionization in interacting galaxies and advanced mergers but not in isolated galaxies. This relation does not show any dependence with the infrared luminosity (i.e. the level of star formation). All this indicates that tidal forces play a key role in the origin of the ionizing shocks in the extra-nuclear regions. We also showed for the first time what appears to be a common log([O i]λ6300/Hα) − log(σ) relation for the extranuclear ionized gas in interacting (U)LIRGs (i.e. covering the entire 10 11.0 −10 12.3 L luminosity range). This preliminary result needs to be investigated further with a larger sample of ULIRGs.

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Statistical Properties of Ultraluminous [ITAL]IRAS[/ITAL] Galaxies from an [ITAL]HST[/ITAL] Imaging Survey

Cited by 52 publications

References 61 publications

Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies

Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

VLT-VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies

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