Warm Molecular Gas in Galaxy-Galaxy Merger NGC 6090

Wang, Junzhi; Zhang, Qizhou; Wang, Zhong; Ho, P. T. P.; Fazio, G. G.; Wu, Yuefang

doi:10.1086/422681

Cited by 16 publications

(16 citation statements)

References 17 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The latter is a more realistic result, given the supporting evidence from Papers I and II and direct observations (e.g., Sanders et al 1988;Dupraz et al 1990;Wang et al 1991Wang et al , 1992Wang et al , 2004Casoli et al 1991;Hibbard et al 1994;Yun & Hibbard 2001).…”

Section: Summary and Discussionmentioning

confidence: 73%

A Survey of Merger Remnants. III. Are Merger Remnants Supported by Rotation or Anisotropy?

Rothberg¹,

Joseph²

2006

Astron J

View full text Add to dashboard Cite

A growing body of observational evidence suggests that the luminosity, photometric shape, and amount of rotational or anisotropic support in elliptical galaxies may provide vital clues to how they formed. Elliptical galaxies appear to fall into two distinct categories based on these parameters: bright, boxy-shaped, and having little or no rotation, and less luminous, disky-shaped, and having significant rotation. One viable formation scenario is the ''merger hypothesis,'' in which two disk galaxies merge to form a new elliptical galaxy. A comparison of the luminosity, photometric shape, and amount of rotation in advanced merger remnants may shed more light on the possible formation scenarios of elliptical galaxies. Yet little observational data exist for such merger remnants. This paper is the third in a series investigating the photometric and kinematic properties of a sample of 51 optically selected advanced merger remnants. Presented here are K-band isophotal shapes and spatially resolved kinematics for a subsample of 37 merger remnants. The results show that $11% of the sample is boxy and anisotropically supported, while $47% is disky and rotationally supported. The remainder of the sample shows variations among expected correlations between shape and rotation. This may suggest that the isophotal shapes are still ''in flux.'' There does appear to be a lower limit to the amount of anisotropy observed in the merger remnants. This may provide an observational diagnostic for discriminating among formation scenarios in elliptical galaxies.

show abstract

Section: Summary and Discussionmentioning

confidence: 73%

A Survey of Merger Remnants. III. Are Merger Remnants Supported by Rotation or Anisotropy?

Rothberg¹,

Joseph²

2006

Astron J

View full text Add to dashboard Cite

show abstract

“…Rigopoulou et al (1996) reported a CO J ¼ 2 1 survey of six ULIRGs, and Yao et al (2003) presented the first survey of CO J ¼ 3 2 emission of LIRGs and ULIRGs from the Scuba Local Universe Galaxy Survey (SLUGS). Recent high-resolution studies of warm, dense molecular gas in individual LIRGs have been performed by Iono et al (2004) and Wang et al (2004).…”

Section: Introductionmentioning

confidence: 99%

Warm, Dense Molecular Gas in the ISM of Starbursts, LIRGs, and ULIRGs

Narayanan

Groppi

Kulesa

et al. 2005

ApJ

View full text Add to dashboard Cite

The role of star formation in luminous and ultraluminous infrared galaxies (LIRGs, L IR ! 10 11 L ; ULIRGs, L IR ! 10 12 L ) is a hotly debated issue: while it is clear that starbursts play a large role in powering the IR luminosity in these galaxies, the relative importance of possible enshrouded AGNs is unknown. It is therefore important to better understand the role of star-forming gas in contributing to the infrared luminosity in IR-bright galaxies. The J ¼ 3 level of 12 CO lies 33 K above ground and has a critical density of $1:5 ; 10 4 cm À3 . The 12 CO J ¼ 3 2 line serves as an effective tracer for warm, dense molecular gas heated by active star formation. Here we report on 12 CO J ¼ 3 2 observations of 17 starburst spiral galaxies, LIRGs, and ULIRGs, which we obtained with the Heinrich Hertz Submillimeter Telescope on Mount Graham, Arizona. Our main results are as follows. (1) We find a nearly linear relation between the infrared luminosity and warm, dense molecular gas such that the infrared luminosity increases as the warm, dense molecular gas to the power 0.92; we interpret this to be roughly consistent with the recent results of Gao & Solomon. (2) We find L IR /M H 2 warm; dense ratios ranging from $38 to $482 L /M using a modified CO-H 2 conversion factor of 8:3 ; 10 19 cm À2 (K km s À1 ) À1 derived in this paper.

show abstract

“…Such a geometry has first been suggested by Kneib et al based on the UV/optical morphology of the potential two nuclei (their regions α and β) and the reddened overlap region (their region γ). Such active overlap regions are often found in nearby interacting systems (e.g., the Antennae: Wilson et al 2000;NGC 6090: Bryant & Scoville 1999;Wang et al 2004).…”

Section: Discussionmentioning

confidence: 98%

Multiple CO lines in SMM J16359+6612 – further evidence for a merger

Weiß

Downes

Walter

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract. Using the IRAM 30 m telescope, we report the detection of the CO(3-2), CO(4-3), CO(5-4) and CO(6-5) lines in the gravitational lensed submm galaxy SMM J16359+6612 at z = 2.5. The CO lines have a double peak profile in all transitions. From a Gaussian decomposition of the spectra we show that the CO line ratios, and therefore the underlying physical conditions of the gas, are similar for the blue and the redshifted component. The CO line Spectral Energy Distribution (SED; i.e. flux density vs. rotational quantum number) turns over already at the CO 5-4 transition which shows that the molecular gas is less excited than in nearby starburst galaxies and high-z QSOs. This difference mainly arises from a lower average H 2 density, which indicates that the gas is less centrally concentrated than in nuclear starburst regions in local galaxies. We suggest that the bulk of the molecular gas in SMM J16359+6612 may arise from an overlap region of two merging galaxies. The low gas density and clear velocity separation may reflect an evolutionary stage of the merger event that is in between those seen in the Antennae and in the more evolved ultraluminous infrared galaxies (ULIRGs) like e.g. Mrk 231.

show abstract

Warm Molecular Gas in Galaxy-Galaxy Merger NGC 6090

Cited by 16 publications

References 17 publications

A Survey of Merger Remnants. III. Are Merger Remnants Supported by Rotation or Anisotropy?

A Survey of Merger Remnants. III. Are Merger Remnants Supported by Rotation or Anisotropy?

Warm, Dense Molecular Gas in the ISM of Starbursts, LIRGs, and ULIRGs

Multiple CO lines in SMM J16359+6612 – further evidence for a merger

Contact Info

Product

Resources

About