Neutral Hydrogen in Arp 158

Iyer, Mansie G.; Simpson, Caroline E.; Gottesman, S. T.; Malphrus, Benjamin K.

doi:10.1086/422731

Cited by 4 publications

(7 citation statements)

References 11 publications

(20 reference statements)

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“…Such a virial mass is close to the molecular mass of Arp 105S for instance (Braine et al 2001). This mass is smaller than the total HI mass in C5 according to Iyer et al (2004). This is not surprising as the HI is more extended.…”

Section: Kinematics Of the Systemmentioning

confidence: 80%

“…The HI data cube was obtained from the literature (Iyer et al 2004 Shallow near-infrared images of the system were obtained from the 2MASS (2 Micron All Sky Survey, Skrutskie et al 2006) archives. They are used exclusively for visual inspection.…”

Section: Himentioning

confidence: 99%

“…The HI data cube was obtained from the literature (Iyer et al 2004). Observations of the atomic hydrogen were performed at the VLA (Very Large Array) in D configuration between 1999-05-14 and 1999-05-17 for a total of 5 h. The velocity resolution is 12.3 km s −1 and the final map resolution is 43.3 ×42.2 corresponding to a physical size of 12.3 kpc×12.6 kpc.…”

Section: Himentioning

confidence: 99%

“…The disks of the galaxies seem to be rather edge-on but their morphology is strongly disturbed making a precise assessment difficult. Radio 21 cm observations have shown that the entire system contains 6.5 × 10 9 M of HI, with column density peaks at the tip of one of the tidal arms and towards the western nucleus (Iyer et al 2004), providing a large reservoir of gas to fuel star formation throughout the system which yields an infrared luminosity of 3.1 × 10 10 L (Sect. 3.3).…”

Section: Introductionmentioning

confidence: 99%

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Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

Boquien¹,

Lisenfeld²,

Duc³

et al. 2011

A&A

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Context. Recent studies have shown that star formation in mergers does not seem to follow the same Schmidt-Kennicutt relation as in spiral disks, presenting a higher star formation rate (SFR) for a given gas column density. Aims. In this paper we study why and how different models of star formation arise. To do so we examine the process of star formation in the interacting system Arp 158 and its tidal debris. Methods. We perform an analysis of the properties of specific regions of interest in Arp 158 using observations tracing the atomic and the molecular gas, star formation, the stellar populations as well as optical spectroscopy to determine their exact nature and their metallicity. We also fit their spectral energy distribution with an evolutionary synthesis code. Finally, we compare star formation in these objects to star formation in the disks of spiral galaxies and mergers. Results. Abundant molecular gas is found throughout the system and the tidal tails appear to have many young stars compared to their old stellar content. One of the nuclei is dominated by a starburst whereas the other is an active nucleus. We estimate the SFR throughout the systems using various tracers and find that most regions follow closely the Schmidt-Kennicutt relation seen in spiral galaxies with the exception of the nuclear starburst and the tip of one of the tails. We examine whether this diversity is due to uncertainties in the manner the SFR is determined or whether the conditions in the nuclear starburst region are such that it does not follow the same Schmidt-Kennicutt law as other regions. Conclusions. Observations of the interacting system Arp 158 provide the first evidence in a resolved fashion that different star-forming regions in a merger may be following different Schmidt-Kennicutt laws. This suggests that the physics of the interstellar medium at a scale no larger than 1 kpc, the size of the largest gravitational instabilities and the injection scale of turbulence, determines the origin of these laws.

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Section: Kinematics Of the Systemmentioning

confidence: 80%

Section: Himentioning

confidence: 99%

Section: Himentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

Boquien¹,

Lisenfeld²,

Duc³

et al. 2011

A&A

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“…For several closely interacting/merging galaxy systems, a number of observational studies have revealed enhanced centrally condensed, as well as widely distributed neutral and molecular gas emissions (e.g., Gordon et al 2001;Casasola et al 2004;Iono et al 2005;Cullen et al 2007;Maybhate et al 2007). HI-observations of merging and interacting galaxies have also been carried out to probe the formation mechanisms of merging and interacting systems (e.g., Iyer et al 2004) and these observations provide vital kinematic information. On average, HI 21-cm emission has been detected from only 25−40% of merging and interacting galaxies observed (e.g.…”

Section: Introductionmentioning

confidence: 99%

Interacting and merging galaxies from the second Byurakan survey

Huchtmeier

Петросян

Krishna

et al. 2008

A&A

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We present new results from HI observations of 53 previously undetected interacting and merging galaxies from the Second Byurakan Survey (SBS), in which 30 systems have been detected (detection rate 56%). High-resolution gray-scale optical images and isophotal maps of the HI detected galaxy systems are presented, in addition to comments on these systems. The possibility of confusion arising from known objects within the telescope beam is discussed for each case. For nine unconfused mergers, global HI parameters are determined. These objects are found to be HI-rich and have normal values of (total) mass-to-luminosity ratios. At least 18 objects in the present sample are found to have radio continuum counterparts above the milli-Jansky level near 1 GHz. Throughout this paper we use a value of H 0 = 72 km s −1 Mpc −1 for the Hubble constant.

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NGC 770: A Counterrotating Core in a Low-Luminosity Elliptical Galaxy

2005

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We present evidence for a counterrotating core in the low-luminosity (M B ¼ À18:2) elliptical galaxy NGC 770 based on internal stellar kinematic data. This counterrotating core is unusual, as NGC 770 is not the primary galaxy in the region and lies in an environment with evidence of ongoing tidal interactions. We discovered the counterrotating core via single-slit Keck ESI echelle spectroscopy; subsequent integral field spectroscopy was obtained with the Gemini Multiobject Spectrograph. The counterrotating region has a peak rotation velocity of 21 km s À1 as compared to the main galaxy's rotation speed of greater than 45 km s À1 in the opposite direction. The counterrotating region extends to a radius of $4 00 (0.6 kpc), slightly smaller than the half-light radius of the galaxy, which is 5B3 (0.8 kpc). The photometry and two-dimensional kinematics suggest that the counterrotating component is confined to a disk whose scale height is less than 0B8 (0.1 kpc). The major axis of counterrotation is misaligned with that of the outer galaxy isophotes by 15 . We compute an age and metallicity of the inner counterrotating region of 3 AE 0:5 Gyr and ½Fe/ H ¼ 0:2 AE 0:2 dex based on Lick absorption-line indices. The lack of other large galaxies in this region limits possible scenarios for the formation of the counterrotating core. We discuss several scenarios and favor one in which NGC 770 accreted a small gas-rich dwarf galaxy during a very minor merging event. If this scenario is correct, it represents one of the few known examples of merging between two dwarf-sized galaxies.

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Neutral Hydrogen in Arp 158

Cited by 4 publications

References 11 publications

Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

Studying the spatially resolved Schmidt-Kennicutt law in interacting galaxies: the case of Arp 158

Interacting and merging galaxies from the second Byurakan survey

NGC 770: A Counterrotating Core in a Low-Luminosity Elliptical Galaxy

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