A CCD Study of the Environment of Seyfert Galaxies. III. Host Galaxies and the Nearby Environments

Virani, S.; Robertis, M. M. De; VanDalfsen, M. L.

doi:10.1086/301586

Cited by 39 publications

(47 citation statements)

References 22 publications

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“…In particular, it was suggested that interacting galaxies or galaxies with companions exhibit a significant excess of nuclear activity compared to isolated galaxies (Dahari 1984;Keel et al 1985;Rafanelli et al 1995). On the other hand, no relation was seen by other studies (Virani et al 2000;Schmitt 2001;Fuentes-Williams & Stocke 1988;MacKenty 1989;Laurikainen & Salo 1995). Hence the issue of possible relations between the environment and nuclear activity appears to be still controversial.…”

Section: Discussionmentioning

confidence: 92%

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

Haan¹,

Schinnerer²,

Mundell³

et al. 2007

The Astronomical Journal

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We present a comprehensive spectroscopic imaging survey of the distribution and kinematics of atomic hydrogen (H i) in 16 nearby spiral galaxies hosting low luminosity active galactic nuclei (AGN), observed with high spectral and spatial resolution (resolution: ∼20 , ∼5 km s −1 ) using the NRAO Very Large Array (VLA). The sample contains a range of nuclear types ranging from Seyfert to star-forming nuclei, and was originally selected for the NUclei of GAlaxies project (NUGA)-a spectrally and spatially resolved interferometric survey of gas dynamics in nearby galaxies designed to identify the fueling mechanisms of AGN and the relation to host galaxy evolution. Here we investigate the relationship between the H i properties of these galaxies, their environment, their stellar distribution, and their AGN type. The large-scale H i morphology of each galaxy is classified as ringed, spiral, or centrally concentrated; comparison of the resulting morphological classification with the AGN type reveals that ring structures are significantly more common in low-ionization narrow emission-line regions (LINER) than in Seyfert host galaxies, suggesting a time evolution of the AGN activity together with the redistribution of the neutral gas. Dynamically disturbed H i disks are also more prevalent in LINER host galaxies than in Seyfert host galaxies. While several galaxies are surrounded by companions (some with associated H i emission), there is no correlation between the presence of companions and the AGN type (Seyfert/LINER).

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Section: Discussionmentioning

confidence: 92%

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

Haan¹,

Schinnerer²,

Mundell³

et al. 2007

The Astronomical Journal

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“…Although past studies have sometimes produced ambiguous results, primarily because of the varying selection criteria of the AGN and control samples, such as morphology and luminosity, the general consensus appears to be that galaxies with active nuclei are more likely to be part of close pairs, possibly inducing nuclear activity through tidal perturbations. At low redshifts, the results have been mixed for Seyfert galaxies ( Dahari 1985;Fuentes-Williams & Stocke 1988;Virani et al 2000). On the other hand, more luminous quasars are usually found in small groups of galaxies, possibly increasing in richness at higher redshifts (e.g., Bahcall et al 1997 for QSOs at z < 0:3; Yee & Green 1987 for z % 0:6).…”

Section: The Local Environmentmentioning

confidence: 99%

The Host Galaxies and Environment of Chandra ‐Selected Active Galactic Nuclei in the Deep ACS GTO Cluster Fields

Martel¹,

Menanteau²,

Tozzi³

et al. 2007

ASTROPHYS J SUPPL S

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We present catalogs and images of optical counterparts to the Chandra-selected X-ray sources found in the fields of the five clusters RX J0152À1357, RX J0849+4452, RDCS J0910+5422, MS 1054À0321, and RDCS J1252À2927, which were imaged with the Advanced Camera for Surveys as part of the ACS Guaranteed Time Observer programs. A total of 98 X-ray sources fall within the ACS mosaics, and positive identifications are made for $96% of them, including confirmed cluster members. We classify the sources as active galactic nuclei (AGNs) or QSOs depending on their X-ray output. The log N (> S ) Ylog S test indicates a significant overdensity of X-ray sources in the RX J0152À 1357, RDCS J0910+5422, and MS 1054À0321 fields with respect to the CDF-S, suggesting an association of some X-ray sources with the large-scale structure of the clusters. From the asymmetry and concentration indices, $52% of the optical counterparts are early-type galaxies, $35% late-type, and the remainder irregular. A blue core is found in approximately half of the early-type galaxies. From visual examination, approximately 40% of the counterparts possess an unresolved nucleus, a common signature of nuclear activity. A majority of these nuclei are found in near faceon late-type galaxies although selection effects might be important. The X-ray to optical flux ratio of the nuclei correlates with the inclination angle of the late-type galaxies but not of the early types, as expected if dust is significant in the circumnuclear regions. The AGNs possess a $50% excess of nearby companions compared to the overall galaxy population in the same fields. The surface density of the X-ray sources is highest at projected radii of P1 Mpc from the cluster center and relatively flat at larger radii. We describe the morphology and environment of the cluster members and compare them with the other optical counterparts.

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“…Quasars Figure 1a displays the versus distribution of M BH L bulge 15 PG quasars (using and H 0 \ 80 km s~1 Mpc~1 ) 0 \ 1). The quasar sample is slightly revised from the L98 sample with the addition of PG 1425]267 from Kirhakos et al (1999) Virani et al (2000). The Spearman rank order correlation coefficient, its signiÐcance level, and the rms scatter are indicated above each panel.…”

Section: The Relationmentioning

confidence: 99%

“…M BH -M bulge The purpose of this paper is to better constrain the slope of the relation using recently published data. M BH -M bulge We use new determinations for 14 nearby galaxies M BH reported in G00 and new bulge luminosity, determi-L bulge , nations for nine Seyfert 1 galaxies by Virani, De Robertis, & VanDalfsen (2000), for which estimates can be M BH (Hb) made. In°2 we review the determination in M BH (Hb) quasars, the new in nearby galaxies, new in M BH L bulge Seyfert galaxies, and the resulting signiÐcantly nonlinear relation.…”

Section: Introductionmentioning

confidence: 99%

On the Linearity of the Black Hole–Bulge Mass Relation in Active and in Nearby Galaxies

Laor

2001

ApJ

136

161

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Analysis of (Palomar-Green) PG quasar observations suggests a nonlinear relation between the black hole mass, and the bulge mass, although a linear relation, as proposed for nearby galaxies, M BH , M bulge , cannot be ruled out. New values for nearby galaxies from K. Gebhardt et al., and measure-M BH L bulge ments for Seyfert 1 galaxies from S. N. Virani et al., are used here to obtain a more accurate value for the slope of the relation. The combined sample of 40 active and nonactive galaxies suggests M BH -M bulge a signiÐcantly nonlinear relation,Further support for a nonlinear relation is provid-M BH P M bulge 1.53B0.14. ed by the slope of the velocity dispersion relation found recently, and by the low found M BH Èstellar M BH in late-type spiral galaxies. The mean ratio is therefore not a universal constant, but rather M BH /M bulge drops from D0.5% in bright ellipticals to D0.05% in low-luminosity bulges.

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A CCD Study of the Environment of Seyfert Galaxies. III. Host Galaxies and the Nearby Environments

Cited by 39 publications

References 22 publications

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

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

The Host Galaxies and Environment of Chandra ‐Selected Active Galactic Nuclei in the Deep ACS GTO Cluster Fields

On the Linearity of the Black Hole–Bulge Mass Relation in Active and in Nearby Galaxies

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