Atomic Hydrogen Properties of Active Galactic Nuclei Host Galaxies: H I in 16 Nuclei of Galaxies (Nuga) Sources

Haan, S.; Schinnerer, E.; Mundell, C. G.; García‐Burillo, S.; Combes, F.

doi:10.1088/0004-6256/135/1/232

Cited by 51 publications

(85 citation statements)

References 75 publications

(109 reference statements)

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“…The majority of the Seyferts with close companions show signs of recent nuclear star formation, leading Storchi‐Bergmann et al to suggest that the pure Seyfert spectrum emerges after the main starburst has faded. A similar evolutionary scenario was suggested by Haan et al (2008), whereby low‐luminosity AGN precede Seyferts after a merger, based on high fractions of the former, but few of the latter in a sample of galaxies with disturbed H i discs. Delays are also implied by the intermediate colours and spectral characteristics of AGN hosts, indicating at least ∼100 Myr between the decline of star formation and black hole activity (Schawinski et al 2009).…”

Section: Introductionsupporting

confidence: 69%

Galaxy pairs in the Sloan Digital Sky Survey - IV. Interactions trigger active galactic nuclei

Ellison¹,

Patton²,

Mendel³

et al. 2011

Monthly Notices of the Royal Astronomical Society

410

421

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Galaxy-galaxy interactions are predicted to cause gas inflows leading to enhanced nuclear star formation. This prediction is borne out observationally, and is also supported by the gas-phase metallicity dilution in the inner regions of galaxies in close pairs. In this paper we test the further prediction that the gas inflows lead to enhanced accretion on to the central supermassive black hole, triggering activity in the nucleus. Based on a sample of 11 060 Sloan Digital Sky Survey galaxies with a close companion (r p < 80 h −1 70 kpc, V < 200 km s −1 ), we classify active galactic nuclei (AGN) based either on emission line ratios or on spectral classification as a quasar. The AGN fraction in the close pairs sample is compared to a control sample of 110 600 mass-and redshift-matched control galaxies with no nearby companion. We find a clear increase in the AGN fraction in close pairs of galaxies with projected separations < 40 h −1 70 kpc by up to a factor of 2.5 relative to the control sample [although the enhancement depends on the chosen signal-to-noise ratio (S/N) cut of the sample]. The increase in AGN fraction is strongest in equal-mass galaxy pairings, and weakest in the lower mass component of an unequal-mass pairing. The increased AGN fraction at small separations is accompanied by an enhancement in the number of 'composite' galaxies whose spectra are the result of photoionization by both AGN and stars. Our results indicate that AGN activity occurs (at least in some cases) well before final coalescence and concurrently with ongoing star formation. Finally, we find a marked increase at small projected separations of the fraction of pairs in which both galaxies harbour AGN. We demonstrate that the fraction of double AGN exceeds the expected random fraction, indicating that some pairs undergo correlated nuclear activity. We discuss some of the factors that have led to conflicting results in previous studies of AGN in close pairs. Taken together with complementary studies, we favour an interpretation where interactions trigger AGN, but are not the only cause of nuclear activity.

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Section: Introductionsupporting

confidence: 69%

Galaxy pairs in the Sloan Digital Sky Survey - IV. Interactions trigger active galactic nuclei

Ellison¹,

Patton²,

Mendel³

et al. 2011

Monthly Notices of the Royal Astronomical Society

410

421

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“…Previous studies have detected H i gas in LINERs (Haan et al 2008;Geréb et al 2013Geréb et al , 2015. Haan et al (2008) found the mean H i mass of seven LINERs to be ∼ 10 10 M , which is comparable to the H i masses of the most massive LIERs in the spectroscopic sample. Figure 5, classification lines are included on each subplot.…”

Section: J2120-39supporting

confidence: 52%

H i galaxies with little star formation: an abundance of LIERs

Parkash

Brown

Jarrett

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a sample of 91 H i galaxies with little or no star formation, and discuss the analysis of the integral field unit (IFU) spectra of 28 of these galaxies. We identified H i galaxies from the H i Parkes All-Sky Survey Catalog (HICAT) with Wide-field Infrared Survey Explorer (WISE) colours consistent with low specific star formation (< 10 −10.4 yr −1 ), and obtained optical IFU spectra with the Wide-Field Spectrograph (WiFeS). Visual inspection of the PanSTARRS, Dark Energy Survey, and Carnegie-Irvine imaging of 62 galaxies reveals that at least 32 galaxies in the sample have low levels of star formation, primarily in arms/rings. New IFU spectra of 28 of these galaxies reveals 3 galaxies with central star formation, 1 galaxy with low-ionisation nuclear emission-line regions (LINERs), 20 with extended low-ionisation emission-line regions (LIERs) and 4 with high excitation Seyfert (Sy) emission. From the spectroscopic analysis of H i selected galaxies with little star formation, we conclude that 75% of this population are LINERs/LIERs.

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“…The stellar mass is derived from the 2MASS K-band images and the K-band mass-to-light ratios (Section 3.2). For the cold gas mass, we use the H i mass of 4.7 × 10 10 M for NGC 1961 (Haan et al 2008), and we estimate the H i mass of about 2 × 10 10 M for NGC 6753 (Haynes & Giovanelli 1984). Since both galaxies are located in poor groups (Fouque et al 1992), the baryon mass of these galaxies should also be included in the baryon budget.…”

Section: Baryon Mass Fractionmentioning

confidence: 99%

Hot X-Ray Coronae Around Massive Spiral Galaxies: A Unique Probe of Structure Formation Models

Bogdán

Forman

Vogelsberger

et al. 2013

ApJ

111

115

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Luminous X-ray gas coronae in the dark matter halos of massive spiral galaxies are a fundamental prediction of structure formation models, yet only a few such coronae have been detected so far. In this paper, we study the hot X-ray coronae beyond the optical disks of two "normal" massive spirals, NGC 1961 and NGC 6753. Based on XMM-Newton X-ray observations, hot gaseous emission is detected to ∼60 kpc-well beyond their optical radii. The hot gas has a best-fit temperature of kT ∼ 0.6 keV and an abundance of ∼0.1 Solar, and exhibits a fairly uniform distribution, suggesting that the quasi-static gas resides in hydrostatic equilibrium in the potential well of the galaxies. The bolometric luminosity of the gas in the (0.05-0.15)r 200 region (r 200 is the virial radius) is ∼6 × 10 40 erg s −1 for both galaxies. The baryon mass fractions of NGC 1961 and NGC 6753 are f b,NGC 1961 ∼ 0.11 and f b,NGC 6753 ∼ 0.09, which values fall short of the cosmic baryon fraction. The hot coronae around NGC 1961 and NGC 6753 offer an excellent basis to probe structure formation simulations. To this end, the observations are confronted with the moving mesh code arepo and the smoothed particle hydrodynamics code gadget. Although neither model gives a perfect description, the observed luminosities, gas masses, and abundances favor the arepo code. Moreover, the shape and the normalization of the observed density profiles are better reproduced by arepo within ∼0.5r 200 . However, neither model incorporates efficient feedback from supermassive black holes or supernovae, which could alter the simulated properties of the X-ray coronae. With the further advance of numerical models, the present observations will be essential in constraining the feedback effects in structure formation simulations.

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Atomic Hydrogen Properties of Active Galactic Nuclei Host Galaxies: H I in 16 Nuclei of Galaxies (Nuga) Sources

Cited by 51 publications

References 75 publications

Galaxy pairs in the Sloan Digital Sky Survey - IV. Interactions trigger active galactic nuclei

Galaxy pairs in the Sloan Digital Sky Survey - IV. Interactions trigger active galactic nuclei

H i galaxies with little star formation: an abundance of LIERs

Hot X-Ray Coronae Around Massive Spiral Galaxies: A Unique Probe of Structure Formation Models

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