Radio survey of Markarian galaxies at 6 and 11 CM

We present deep images of the kpc-scale radio continuum emission in 14 edge-on galaxies (ten Seyfert and four starburst galaxies). Observations were taken with the VLA at 4.9 GHz (6 cm). The Seyfert galaxies were selected from a distance-limited sample of 22 objects (defined in paper I). The starburst galaxies were selected to be well-matched to the Seyferts in radio power, recessional velocity and inclination angle. All four starburst galaxies have a very bright disk component and one (NGC 3044) has a radio halo that extends several kpc out of the galaxy plane. Six of the ten Seyferts observed have large-scale (radial extent ∼ >1 kpc) radio structures extending outward from the nuclear region, indicating that large-scale outflows are quite common in Seyferts.Large-scale radio sources in Seyferts are similar in radio power and radial extent to radio halos in edge-on starburst galaxies, but their morphologies do not resemble spherical halos observed in starburst galaxies. The sources have diffuse morphologies, but, in general, they are oriented at skewed angles with respect to the galaxy minor axes. This result is most easily understood if the outflows are AGN-driven jets that are somehow diverted away from the galaxy disk on scales ∼ >1 kpc. Starburst-driven winds, however, cannot be ruled out. More observational work is needed to determine whether massive star formation is present at high enough rates to drive galactic winds out to kpc scales in Seyfert galaxies.

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“…Previous workers (e.g., Kojoian et al 1980, Mulchaey et al 1995 have observed this galaxy, but also failed to detect it.…”

Section: Mrk 577mentioning

confidence: 73%

Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission

Colbert¹,

Baum²,

Gallimore³

et al. 1996

ApJ

108

130

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“… REFERENCES: (1) Ulvestad, Antonucci & Goodrich (1995); (2) Leighly (1999); (3) Wang & Lu (2001); (4) Ho (2002); (5) Weaver, Gelbord & Yaqoob (2001); (6) Nandra et al (1997); (7) Corbel et al (2003); (8) Hynes et al (2003); (9) Fabbiano et al (2003); (10) Tremaine et al (2002); (11) Sambruna et al (1999); (12) Pellegrini et al (2003); (13) Saglia et al (1993); (14) Polletta et al (1996); (15) Bassani et al (1999); (16) Woo & Urry (2002); (17) Gondoin et al (2002); (18) Zhou & Wang (2002); (19) Thean et al (2001); (20) Pounds et al (2001); (21) Kaspi et al (2000); (22) Ho & Peng (2001); (23) Gregory & Condon (1991); (24) Terashima et al (2002); (25) Griffith et al (1995); (26) Simien & Prugniel (2002) and HYPERLEDA Catalogue: http://www-obs.univ-lyon1.fr/hypercat/; (27) Ho & Ulvestad (2001); (28) Ho et al (2001); (29) Nagar et al (2002a); (30) Barth, Ho & Sargent (2002); (31) Terashima & Wilson (2003); (32) Allen et al (2001); (33) Héraudeau & Simien (1998); (34) Churazov et al (2003); (35) Fabbiano, Kim & Trincheri (1992); (36) Shih, Iwasaw & Fabian (2003); (37) Loewenstein et al (2001); (38) Merritt & Ferrarese (2001); (39) Di Matteo et al (2003); (40) Giovannini et al (1998); (41) Di Matteo et al (2001); (42) De Rosa, Fabian & Piro (2002); (43) George et al (2000); (44) Lawson & Turner (1997); (45) Moran et al (2001); (46) Dhawan et al (2000); (47) Frontera et al (2001); (48) Wagner et al (2001); (49) Rush, Malkan & Edelson (1996); (50) Becker, White & Edwards (1991); (51) Kojoian et al (1980); (52) White, Giommi & Angelini (2000); (53) Véron‐Cetty & Véron (2001); (54) Falcke et al (2000); (55) Ulvestad & Wilson (1989); (56) Falcke, Malkan & Biermann (1995); (57) Turner & Pounds (1989); (58) Tadhunter et al (2003); (59) …”

Section: The Samplementioning

confidence: 99%

A Fundamental Plane of black hole activity

Merloni

Heinz

Matteo

2003

Monthly Notices of the Royal Astronomical Society

1,220

116

1,822

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We examine the disc–jet connection in stellar mass and supermassive black holes by investigating the properties of their compact emission in the X‐ray and radio bands. We compile a sample of ∼100 active galactic nuclei with measured masses, 5‐GHz core emission, and 2–10 keV luminosities, together with eight galactic black holes with a total of ∼50 simultaneous observations in the radio and X‐ray bands. Using this sample, we study the correlations between the radio (LR) and the X‐ray (LX) luminosity and the black hole mass (M). We find that the radio luminosity is correlated with bothM and LX, at a highly significant level. In particular, we show that the sources define a ‘Fundamental Plane’ in the three‐dimensional (log LR, log LX, log M) space, given by log LR= (0.60+0.11−0.11) log LX+ (0.78+0.11−0.09) log M+ 7.33+4.05−4.07, with a substantial scatter of σR= 0.88. We compare our results to the theoretical relations between radio flux, black hole mass, and accretion rate derived by Heinz & Sunyaev. Such relations depend only on the assumed accretion model and on the observed radio spectral index. Therefore, we are able to show that the X‐ray emission from black holes accreting at less than a few per cent of the Eddington rate is unlikely to be produced by radiatively efficient accretion, and is marginally consistent with optically thin synchrotron emission from the jet. On the other hand, models for radiatively inefficient accretion flows seem to agree well with the data.

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“…Part of a sample of Seyfert galaxies that were surveyed for neutral hydrogen by Mirabel & Wilson (1984). This galaxy is also part of a radio survey of Markarian galaxies at 6 and 11 cm by Kojoian et al (1980) as well as part of a compact radio core sample surveyed by Giuricin et al (1990). NGC 1143/4.…”

Section: A P P E N D I X Amentioning

confidence: 99%

Molecular gas properties of 12-μm Seyfert galaxies - I. The southern sample

Strong

Pedlar

Aalto

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We have used the 15‐m Swedish European Southern Observatory (ESO) Submillimetre Telescope (SEST) to observe the J= 1 → 0 and J= 2 → 1 transition lines of CO in 30 Southern hemisphere Seyfert galaxies from the extended 12‐μm sample of Rush, Malkan & Spinoglio. We detected CO J= 1 → 0 in 16 out of the 30 Seyfert galaxies and CO J= 2 → 1 in 17 out of the 30 Seyfert galaxies. From the observed spectra, various CO gas properties have been derived including the luminosity of the CO gas and, using a standard conversion factor, the H2 mass. The average H2 gas mass for Seyfert 1 galaxies was 3 × 109 M⊙ for CO J= 1 → 0 and 1 × 109 M⊙ for CO J= 2 → 1, while in comparison the H2 gas mass for Seyfert 2 type galaxies was 11 × 109 M⊙ for CO J= 1 → 0 and 3 × 109 M⊙CO J= 2 → 1. From this small sample of Seyfert galaxies, we tentatively support the conclusion that type 2 Seyfert galaxies contain more molecular gas than their type 1 counterparts.

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Radio survey of Markarian galaxies at 6 and 11 CM

Cited by 14 publications

References 0 publications

Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission

Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission

A Fundamental Plane of black hole activity

Molecular gas properties of 12-μm Seyfert galaxies - I. The southern sample

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