Markarian 348: A Tidally Disturbed Seyfert Galaxy

Simkin, S. M.; Su, Hongjun; Gorkom, Jacqueline van; Hibbard, J. E.

doi:10.1126/science.235.4794.1367

Cited by 37 publications

(32 citation statements)

References 25 publications

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“…Evidence of the existence of such reservoir can be seen in the HI gas distribution around galaxies (e.g. Simkin et al 1987, Tilanus & Allen 1993, extending further out than the UV-disks, and could well be the source for such cosmic accretion (Sancisi et al 2008). These would support the inside-out disk growth scenario.…”

Section: Introductionsupporting

confidence: 51%

UV-IR color profiles of the outer regions of 2K nearby S⁴G galaxies

Bouquin

Paz

2016

Proc. IAU

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Abstract. We present our new, spatially-resolved, photometry in FUV and NUV from images obtained by GALEX, and IRAC1 (3.6 µm) photometry obtained by the Spitzer Space Telescope. We analyzed the surface brightness profiles µFUV, µNUV, µ [3.6] , as well as the radial evolution of the (FUV-NUV), ), and (NUV -[3.6]) colors in the Spitzer Survey of Stellar Structures in Galaxies (S 4 G) galaxies (d<40 Mpc) sample. We defined the GALEX Blue Sequence (GBS) and GALEX Red Sequence (GBR) from the (FUV -NUV) versus (NUV -[3.6]) colorcolor diagram, populated by late-type star forming galaxies and quiescent early-type galaxies respectively. While most disk becomes radially bluer for GBS galaxies, and stay constant for GRS galaxies, a large fraction (>50%) of intermediary GALEX Green Valley (GGV) galaxies' outer disks are becoming redder. An outside-in quenching mechanism such as environmentally-related mechanisms such as starvation or ram-pressure-stripping could explain our results.

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Section: Introductionsupporting

confidence: 51%

UV-IR color profiles of the outer regions of 2K nearby S⁴G galaxies

Bouquin

Paz

2016

Proc. IAU

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“…UGC 508 (NGC 266) lies about 23 to the northeast of UGC 499; the peculiar structure of the gas in UGC 499 might be a result of a past interaction with its neighbour. The H properties of UGC 499 were discussed in detail by Heckman et al (1982) and Simkin et al (1987). UGC 624 (NGC 338) is one of the most lopsided galaxies in our sample, both in the gas distribution and in the kinematics.…”

Section: Notes On Individual Galaxiesmentioning

confidence: 97%

The Westerbork HI survey of spiral and irregular galaxies

Noordermeer¹,

Hulst²,

Sancisi

et al. 2005

A&A

193

272

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We present H observations of 68 early-type disk galaxies from the WHISP survey. They have morphological types between S0 and Sab and absolute B-band magnitudes between -14 and -22. These galaxies form the massive, high surface-brightness extreme of the disk galaxy population, few of which have been imaged in H before. The H properties of the galaxies in our sample span a large range; the average values of M HI /L B and D HI /D 25 are comparable to the ones found in later-type spirals, but the dispersions around the mean are larger. No significant differences are found between the S0/S0a and the Sa/Sab galaxies. Our early-type disk galaxies follow the same H mass-diameter relation as later-type spiral galaxies, but their effective H surface densities are slightly lower than those found in later-type systems. In some galaxies, distinct rings of H emission coincide with regions of enhanced star formation, even though the average gas densities are far below the threshold of star formation derived by Kennicutt (1989, ApJ, 344, 685). Apparently, additional mechanisms, as yet unknown, regulate star formation at low surface densities. Many of the galaxies in our sample have lopsided gas morphologies; in most cases this can be linked to recent or ongoing interactions or merger events. Asymmetries are rare in quiescent galaxies. Kinematic lopsidedness is rare, both in interacting and isolated systems. In the appendix, we present an atlas of the H observations: for all galaxies we show H surface density maps, global profiles, velocity fields and radial surface density profiles.

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“…Since the H i gas extends in most disk galaxies much further than the optical disk, it is more loosely bound in the outer region because of the decrease of the gravitational potential. Hence, it provides an ideal tool to identify interactions and tidal features (e.g., Simkin et al 1987;Mundell et al 1995). Furthermore, due to its dissipative nature the gas is more sensitive to dynamical disturbances, either internal, such as non-axisymmetric potentials, or external, such as tidal interactions.…”

Section: Introductionmentioning

confidence: 99%

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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Markarian 348: A Tidally Disturbed Seyfert Galaxy

Cited by 37 publications

References 25 publications

UV-IR color profiles of the outer regions of 2K nearby S⁴G galaxies

UV-IR color profiles of the outer regions of 2K nearby S⁴G galaxies

The Westerbork HI survey of spiral and irregular galaxies

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

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Markarian 348: A Tidally Disturbed Seyfert Galaxy

Cited by 37 publications

References 25 publications

UV-IR color profiles of the outer regions of 2K nearby S4G galaxies

UV-IR color profiles of the outer regions of 2K nearby S4G galaxies

The Westerbork HI survey of spiral and irregular galaxies

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

Contact Info

Product

Resources

About

UV-IR color profiles of the outer regions of 2K nearby S⁴G galaxies

UV-IR color profiles of the outer regions of 2K nearby S⁴G galaxies