O. Yam

University of Quintana Roo

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H. M. Tovmassian

Glendale Community College

H. Tiersch

Stuttgart Observatory

O. Martı́nez

Benemérita Universidad Autónoma de Puebla

Timothy A. D. Paglione

York College, City University of New York

L. Carrasco

Tecnológico de Monterrey

Luis F. Rodrı́guez

Autonomous University of Chiapas

H. Bravo

A. Carramiñana

National Institute of Astrophysics, Optics and Electronics

Tomoka Tosaki

Joetsu University of Education

L. Bronfman

University of Chile

Cooperative Institutions

Universidad Nacional Autónoma de México

National Institute of Astrophysics, Optics and Electronics

Max Planck Society

Instituto de Geofísica y Astronomía

Centre National de la Recherche Scientifique

Center for Astrophysics Harvard & Smithsonian

University of Canterbury

Max Planck Institute for Radio Astronomy

Nagoya University

Harvard University

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Dynamics of Hickson Compact Groups of Galaxies

H. M. Tovmassian V. Chavushyan O. Martı́nez O. Yam H. Tiersch

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The Nature of Compact Groups

International Astronomical Union Colloquium (2000)

H. M. Tovmassian H. Tiersch O. Martı́nez O. Yam

Abstract We show that compact groups (CGs) are real physical entities, that almost all HCGs are dynamically associated with generally elongated loose groups of galaxies, that HCGs are compact cores of loose groups, and that they are longer living formations.

10.1017/s0252921100055056

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Dynamics of HCGs

arXiv (Cornell University) (2002)

H. M. Tovmassian V. H. Chavushian O. Martı́nez O. Yam H. Tiersch

It is shown that compact groups of galaxies (HCGs, ShCGS) are stable formations, in which principal member galaxies together with faint galaxies in their environment rotate in elongated orbits around the common gravitational center of the group. Hence, the multitude of puzzles related to CGs: the very existence of CGs, absence of strong radio sources, absence of strong signs of interaction and merging, the fact that elliptical members (the best candidates for ongoing merging) are not more frequently first-ranked than spirals, etc., are solved. The number of such groups, may be much higher in the near Universe, since only those of them, the elongation of which is oriented close to the line of sight, or bright members of which happen to be close to each other during regular rotation, are detected as the so-called compact groups.

10.48550/arxiv.astro-ph/0203066

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THE RADIO JET ASSOCIATED WITH THE MULTIPLE V380 ORI SYSTEM

The Astronomical Journal (2016)

Luis F. Rodrı́guez O. Yam Carlos Carrasco‐González Guillem Anglada Alfonso Trejo

The giant Herbig-Haro object 222 extends over $\sim$6$'$ in the plane of the sky, with a bow shock morphology. The identification of its exciting source has remained uncertain over the years. A non-thermal radio source located at the core of the shock structure was proposed to be the exciting source. However, Very Large Array studies showed that the radio source has a clear morphology of radio galaxy and a lack of flux variations or proper motions, favoring an extragalactic origin. Recently, an optical-IR study proposed that this giant HH object is driven by the multiple stellar system V380 Ori, located about 23$'$ to the SE of HH 222. The exciting sources of HH systems are usually detected as weak free-free emitters at centimeter wavelengths. Here we report the detection of an elongated radio source associated with the Herbig Be star or with its close infrared companion in the multiple V380 Ori system. This radio source has the characteristics of a thermal radio jet and is aligned with the direction of the giant outflow defined by HH~222 and its suggested counterpart to the SE, HH~1041. We propose that this radio jet traces the origin of the large scale HH outflow. Assuming that the jet arises from the Herbig Be star, the radio luminosity is a few times smaller than the value expected from the radio-bolometric correlation for radio jets, confirming that this is a more evolved object than those used to establish the correlation.

Herbig–Haro object

Outflow

X-shaped radio galaxy

Young stellar object

10.3847/0004-6256/152/4/101

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On the X-Ray Emission of the Low-Mass Galaxy Groups

The Astrophysical Journal (2002)

H. M. Tovmassian O. Yam H. Tiersch

It is shown that low-mass groups obey the LX ~ σ law deduced for galaxy clusters. The impression of the more shallow slope of the LX-σv correlation for groups is created not by enhanced X-ray emission, but by the underestimation of the radial velocity dispersion of some groups.

Velocity dispersion

Radial velocity

10.1086/339769

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Citations (9)

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International Astronomical Union Colloquium (2004)

Helmut A. Abt Arcadio Poveda J. L. Halbwachs M. Mayor S. Udry

An abstract is not available for this content so a preview has been provided. As you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Content (measure theory)

10.1017/s0252921100008903

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The Structure, Kinematics, and Physical Properties of the Molecular Gas in the Starburst Nucleus of NGC 253

The Astrophysical Journal (2004)

Timothy A. D. Paglione O. Yam Tomoka Tosaki James M. Jackson

We present 52 × 26 resolution interferometry of CO J = 1 → 0 emission from the starburst galaxy NGC 253. The high spatial resolution of these new data, in combination with recent high-resolution maps of 13CO, HCN, and near-infrared emission, allow us for the first time to link unambiguously the gas properties in the central starburst of NGC 253 with its bar dynamics. We confirm that the star formation results from bar-driven gas flows as seen in "twin peaks" galaxies. Two distinct kinematic features are evident from the CO map and position-velocity diagram: a group of clouds rotating as a solid body about the kinematic center of the galaxy and a more extended gas component associated with the near-infrared bar. We model the line intensities of CO, HCN, and 13CO to infer the physical conditions of the gas in the nucleus of NGC 253. The results indicate increased volume densities around the radio nucleus in a twin peaks morphology. Compared with the CO kinematics, the gas densities appear highest near the radius of a likely inner Linblad resonance and slightly lead the bar minor axis. This result is similar to observations of the face-on, twin peaks galaxy NGC 6951 and is consistent with models of starburst generation due to gas inflow along a bar.

Bar (unit)

Barred spiral galaxy

10.1086/422354

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Citations (35)

On the X-ray emission of the low-mass galaxy groups

arXiv (Cornell University) (2002)

H. M. Tovmassian O. Yam H. Tiersch

It is shown that the low-mass groups obey the $L_{x}\simσ_v^{4}$ law deduced for galaxy clusters. The impression of the more shallow slope of the $L_x-σ_{v}$ correlation for groups is created not by enhanced X-ray emission, but by underestimation of the radial velocity dispersion of some groups.

Velocity dispersion

10.48550/arxiv.astro-ph/0201332

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The uvby-beta Photoelectric Photometry and Spectroscopy of the Open Cluster NGC 1342

R. Peniche H. Bravo L. J. Corral I. Hirata O. Yam

Photoelectric effect

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Dynamics of HCGs

arXiv (Cornell University) (2002)