Multicolor surface photometry of powerful radio galaxies. II - Morphology and stellar content

Smith, Eric P.; Heckman, Timothy M.

doi:10.1086/167524

Cited by 112 publications

(131 citation statements)

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“…O'Dea et al (1996) find that 13% of the optical hosts of GPS sources have companions in their sample of 30 objects. Smith & Heckman (1989) find that 20% of the hosts in their sample of powerful radio galaxies have a companion. The hosts of CSS/GPS sources without a companion also show signs of interaction.…”

Section: Morphologg Iesmentioning

confidence: 99%

“…The fit is described by eA ¼ 17:69 þ 4:69 log R eA . The slope of the fit, ¼ 4:69, is steeper than that usually seen among normal ellipticals and radio galaxies ( $ 3:0;e.g., Kormendy 1977;Hamabe & Kormendy 1987;Smith & Heckman 1989). However, slopes of up to $ 5 have been seen in samples of non-BCGs and CSS/GPS sources.…”

Section: Model Fits To Surface Brigg Htnessmentioning

confidence: 99%

“…The optical hosts of classical radio galaxies and radioloud quasars are generally luminous (>L*) massive elliptical galaxies (e.g., Govoni et al 2000;Dunlop et al 2003). There is some evidence that radio galaxy hosts have undergone mergers or tidal interactions with other galaxies (Smith & Heckman 1989), which may provide fuel for the radio source. Many of the hosts of powerful GPS sources also appear to be mergers, though not the high fraction that is seen in ULIRGs (O'Dea et al 1996).…”

Section: Introductionmentioning

confidence: 99%

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Radio-ExcessIRASGalaxies. II. Host Galaxies

2004

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This is the second of a series of papers studying a sample of radio-excess IRAS galaxies. These galaxies have radio emission in excess of that expected due to star formation, but largely fall between the traditional categories of radio-loud and radio-quiet active galaxies. R-band images of the hosts of far-infrared ( FIR)-luminous radioexcess galaxies are presented and analyzed. The hosts of the FIR-luminous radio-excess galaxies are luminous galaxies, on average 0.8 mag brighter than M Ã R . Their optical luminosities and morphologies are similar to comparison samples of radio-loud compact steep-spectrum and gigahertz peaked-spectrum sources and extended radio galaxies. We find a similar fraction of galaxies in our sample ($70%) with companions or distorted morphologies as in radio-loud comparison samples. This is consistent with radio activity being associated with tidal interaction. The majority (65%) of the FIR-luminous radio-excess galaxies have radio source sizes that are smaller than the optical host by more than an order of magnitude. These compact radio sources may be young precursors to classical radio galaxies or a different population of radio sources, possibly confined by the host interstellar medium. The host galaxy types were determined by analysis of the surface brightness distributions. The elliptical hosts have effective surface brightnesses and radii consistent with known ellipticals but inconsistent with a population of brightest cluster galaxies. Thus, it is unlikely these objects are the precursors of FR I radio galaxies. The disk hosts have smaller sizes and low radio excesses. However, they have a range of radio source sizes, which is not expected if they are radio-''loud'' Seyfert galaxies.

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Section: Morphologg Iesmentioning

confidence: 99%

Section: Model Fits To Surface Brigg Htnessmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Radio-ExcessIRASGalaxies. II. Host Galaxies

2004

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“…Heckman et al 1986;Smith & Heckman 1989;De Koff et al 1996;Verdoes Klein et al 1999; Send offprint requests to: R. Morganti, e-mail: morganti@nfra.nl Based on observations with the Westerbork Synthesis Radio Telescope (WSRT) and the Very Large Array (VLA).…”

Section: Gas In and Around Radio Galaxiesmentioning

confidence: 99%

Large-scale gas disk around the radio galaxy Coma A

Morganti¹,

Oosterloo²,

Tinti

et al. 2002

A&A

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Abstract. We present WSRT and VLA radio observations of the neutral hydrogen in the radio galaxy Coma A. We detect extended H I absorption against both radio lobes of Coma A, at distances of about 30 kpc from the centre. Coma A is the first radio galaxy in which H I is seen in absorption at such large distances from the nucleus. The match between the velocities of the neutral hydrogen and those of the extended ionized gas suggests that they are part of the same disk-like structure of at least 60 kpc in diameter. Most likely, this gas disk is partly ionised by the bulk motion of the radio lobes expanding into it. The gas mass of this disk is at least 10 9 M . The relatively regular structure of the gas disk suggests that a merger occurred involving at least one large gas-rich galaxy, at least a few times 10 8 yr ago.Key words. galaxies: ISM -galaxies: active -radio lines: galaxies 1. Gas in and around radio galaxies Many early-type galaxies in the nearby universe appear to have experienced a recent merger/accretion event. In many cases, this has involved at least one gas-rich companion/galaxy that has brought a significant amount of gas into the galaxy. Indeed, H I, FIR and CO observations of elliptical galaxies have demonstrated that many of these objects have an active and interesting cold interstellar medium, often qualitatively (and sometime also quantitatively) similar to that observed in spirals (see Knapp 1999 for a review). Gas is a key factor in determining the evolution of early-type galaxies (e.g. Kauffmann 1996). Among early-type galaxies, gas-rich systems may represent an important phase in the evolution that many elliptical galaxies go through and they give important information on the formation and evolution of these systems.Apart from being important for the overall evolution of early-type galaxies, there is also compelling morphological and kinematical evidence that the activity in powerful radio galaxies is triggered by galaxy mergers and interactions (e.g. Heckman et

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“…Many classical radio galaxies and QSOs have been observed at optical and near-infrared wavelengths to have double-nuclei, tidal bridges/tails, and close companions consistent with them being the mergers of disk galaxies (e.g., Stockton & MacKenty 1983;Heckman et al 1986;Smith & Heckman 1989a, 1989bMcLeod & Rieke 1994;Surace et al 2001). Further evidence of the AGN-merger connection has resulted from multiwavelength surveys of luminous infrared-selected galaxies, which have shown these galaxies to be merging/interacting disk galaxies and have shown an increasing fraction of infrared galaxies with optical, near-infrared, and X-ray signatures of imbedded AGNs as a function of increasing luminosity (e.g., Sanders et al 1988bSanders et al , 1988cVeilleux et al 1997, Veilleux et al 1999aVignati et al 1999).…”

Section: Introductionmentioning

confidence: 99%

Untitled

2005

ASTROPHYS J SUPPL S

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This paper reports the latest results from a millimeter-wave (CO) spectroscopic survey of IRAS-detected radio galaxies with L 1:4 GHz $ 10 23 10 28 W Hz À1 in the redshift range z $ 0:02 0:15. The IRAS flux-limited sample contains 33 radio galaxies with different radio morphologies and a broad range of infrared luminosities (L IR ¼ 10 9 10 12 L ), allowing for an investigation of (1) whether low-z radio-selected active galactic nuclei (AGNs) reside in molecular gas-rich host galaxies and (2) whether the CO properties are correlated with the properties of the host galaxy or the AGN. All of the radio galaxies in Mazzarella et al. and Mirabel et al. have been reobserved. Three new CO detections have been made, raising the total number of CO detections to nine and setting the survey detection rate at $25%. Many of the CO lines have double-peaked profiles, and the CO line widths are broad (average Áv FWHM $ 500 AE 130 km s À1 ), exceeding the average CO widths of both ultraluminous infrared galaxies (300 AE 90 km s À1 ) and Palomar-Green QSOs (260 AE 160 km s À1 ), and thus being indicative of massive host galaxies. The CO luminosities translate into molecular gas masses of $(0:4 7) ; 10 9 M , however, the 3 CO upper limits for nondetections do not rule out a molecular gas mass as high as that of the Milky Way ($3 ; 10 9 M ). Optical images of eight out of nine molecular gas-rich radio galaxies show evidence of close companions and/or tidal features. Finally, there is no obvious correlation between radio power and molecular gas mass. However, it is notable that only one F-R II galaxy out of 12 is detected in this CO survey; the remaining detections are of galaxies hosting F-R I and compact radio jets.

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Multicolor surface photometry of powerful radio galaxies. II - Morphology and stellar content

Cited by 112 publications

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Radio-ExcessIRASGalaxies. II. Host Galaxies

Radio-ExcessIRASGalaxies. II. Host Galaxies

Large-scale gas disk around the radio galaxy Coma A

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