The cold gas properties of Markarian galaxies

Kandalyan, R. A.

doi:10.1051/0004-6361:20021701

Cited by 20 publications

(23 citation statements)

References 32 publications

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“…The type Ic SN2002jj (Foley & Filippenko 2002) is positioned very close to the nuclear region. Kandalyan (2003) this galaxy is a strong source of neutral HI and molecular H 2 , and CO emissions and a source of 1.4 GHz continuum radio emission (Condon et al 1998). Our morphological study confirms the Sa spiral structure of this object.…”

Section: The Morphological Classificationmentioning

confidence: 96%

Early-type galaxies with core collapse supernovae

Hakobyan¹,

Петросян²,

McLean

et al. 2008

A&A

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Aims. It is widely accepted that the progenitors of core collapse SNe are young massive stars and therefore their host galaxies are mostly spiral or irregular galaxies dominated by a young stellar population. Surprisingly, among morphologically classified hosts of core collapse SNe, we find 22 cases where the host has been classified as an Elliptical or S0 galaxy. Methods. To clarify this apparent contradiction, we carry out a detailed morphological study and an extensive literature search for additional information on the sample objects. Results. Our results are as follows: 1. Of 22 "early type" objects, 17 are in fact misclassified spiral galaxies, one is a misclassified irregular, and one is a misclassified ring galaxy. 2. Of the 3 objects maintaining the early type classification, one (NGC 2768) is a suspected merger remnant, another (NGC 4589) is definitely a merger, and the third (NGC 2274) is in close interaction. The presence of some amount of young stellar population in these galaxies is therefore not unexpected. Conclusions. These results confirm the presence of a limited, but significant, number of core collapse SNe in galaxies generally classified as early-type. In all cases, anyway, there are independent indicators of the presence in host galaxies of recent star formation due to merging or gravitational interaction.

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Section: The Morphological Classificationmentioning

confidence: 96%

Early-type galaxies with core collapse supernovae

Hakobyan¹,

Петросян²,

McLean

et al. 2008

A&A

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“…They derive for either galaxy a neutral gas mass M HI ∼ 5 × 10 9 M . A subsequent work of Kandalyan (2003), taking into account radio CO line observations, indicates that NGC 7679 possesses a comparable amount of molecular hydrogen (M H2 ∼ 6 × 10 9 M ).…”

Section: Radio Observationsmentioning

confidence: 97%

“…Since the CO gas kinematics reveals the rotation and/or velocity dispersion close to the nucleus, this phenomenon is interpreted as due to a rapidly rotating nuclear disk (cf. Kandalyan 2003). As such, part of this circumnuclear gas is likely prone to streaming inward with velocities ∼100 km s −1 directly onto the nucleus (cf.…”

Section: Ngc 7679 In the Framework Of The Agn-starburst Connection Issuementioning

confidence: 99%

NGC 7679: an anomalous, composite Seyfert 1 galaxy whose X-ray luminous AGN vanishes at optical wavelengths

Buson¹,

Cappellari

Corsini

et al. 2006

A&A

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Morphological disturbances and gas kinematics of the SB0 galaxy NGC 7679 = Arp 216 are investigated to understand the history of this highly composite object, where AGN and starburst signatures dominate in the X-ray and optical/IR regime, respectively. Perturbations of the ionized gas velocity field appear quite mild within 15 (∼5 kpc) of the center, so it can be straightforwardly modeled as a circularly rotating disk. Outside that radius, significant disturbances are seen. In particular, the eastern distorted arm as well as the huge neutral hydrogen bridge connecting NGC 7679 to the nearby Seyfert spiral NGC 7682 unambiguously represent the vestige of a close encounter of the two objects ∼500 Myr ago. The relationship of such a past event with the much more recent, centrally located starburst (not older than 20 Myr) cannot be easily established. Together, the classification of NGC 7679 is less extreme than that proposed in the past, being simply a (disturbed) galaxy where starburst and AGN activity coexist with a starburst dominating the bolometric luminosity.

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“…c Absolute K-band magnitude (Rothberg & Joseph 2004). d Total mass of neutral atomic hydrogen gas, taken from compilation by Kandalyan (2003). e Total star formation rate (U et al 2012).…”

Section: Ngc 1614 and Ngc 34: A Tale Of Two Lirgsmentioning

confidence: 99%

Alma Observations of Warm Dense Gas in NGC 1614—breaking of the Star Formation Law in the Central Kiloparsec

Cao

et al. 2015

ApJ

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We present ALMA Cycle-0 observations of the CO (6-5) line emission and of the 435 μm dust continuum emission in the central kiloparsec of NGC 1614, a local luminous infrared galaxy at a distance of 67.8 Mpc (1 = 329 pc). The CO emission is well resolved by the ALMA beam (0. 26 × 0. 20) into a circumnuclear ring, with an integrated flux of f = 898 (±153) Jy km s −1 , which is 63(±12)% of the total CO (6-5) flux measured by Herschel. The molecular ring, located between 100 pc < r < 350 pc from the nucleus, looks clumpy and includes seven unresolved (or marginally resolved) knots with median velocity dispersion of ∼40 km s −1 . These knots are associated with strong star formation regions with Σ SFR ∼ 100 M yr −1 kpc −2 and Σ Gas ∼ 10 4 M pc −2 . The nondetections of the nucleus in both the CO (6-5) line emission and the 435 μm continuum rule out, with relatively high confidence, a Compton-thick active galactic nucleus in NGC 1614. Comparisons with radio continuum emission show a strong deviation from an expected local correlation between Σ Gas and Σ SFR , indicating a breakdown of the Kennicutt-Schmidt law on the linear scale of ∼100 pc.

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The cold gas properties of Markarian galaxies

Cited by 20 publications

References 32 publications

Early-type galaxies with core collapse supernovae

Early-type galaxies with core collapse supernovae

NGC 7679: an anomalous, composite Seyfert 1 galaxy whose X-ray luminous AGN vanishes at optical wavelengths

Alma Observations of Warm Dense Gas in NGC 1614—breaking of the Star Formation Law in the Central Kiloparsec

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