Hostname: page-component-745bb68f8f-b6zl4 Total loading time: 0 Render date: 2025-01-25T19:50:41.174Z Has data issue: false hasContentIssue false
  • English
  • Français

Statistical Properties of the Mid and Far IR Emission in Mixed Morphology (E+S) Pairs of Galaxies

Published online by Cambridge University Press:  12 April 2016

H. M. Hernández Toledo ,
D. Dultzin-Hacyan  and
J. W. Sulentic
H. M. Hernández Toledo
Affiliation:
Instituto de Astronomía, UNAM Apdo. 70-264, MéxicoD. F., 04510
D. Dultzin-Hacyan
Affiliation:
Instituto de Astronomía, UNAM Apdo. 70-264, MéxicoD. F., 04510
J. W. Sulentic
Affiliation:
Department of Physics and Astronomy, University of Alabama, TuscaloosaAL 35487

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report the results of a detailed statistical analysis of the Mid and Far IR (MIR/FIR) emission properties in a mixed morphology (E+S) sample of galaxy pairs from the Karachentsev (1972) Catalogue. The sample is large and diverse enough (≃ 130 pairs) to permit discrimination of pairs by morphological types and interaction classes. It samples a large enough volume to enable a non-parametric estimate of a Far-Infrared Luminosity Function (FIRLF). We find average factors of 3 and 5 enhancement in FIR and 25μm luminosities of the late-type pair components relative to an isolated galaxy control sample from Karachentseva (1973) Catalogue. This is interpreted as the MIR/FIR signature of the link between interaction and star formation. Although the spirals in (E+S) pairs fail to show a trend towards higher FIR luminosity with decreasing companion separation, a high-order comparison that takes into account information on the interaction classes, morphological types and the HI content suggests that:

  1. • a clear correlation between the IR luminosities and interaction classes is present suggesting that a subsample of the (E+S) pairs is more closely related to recent events of star formation,

  2. • the ratio of present to past star formation (as measured by the IR luminosities scaled to LB luminosity), increases measurably along the sequence Sa-Sc in paired spirals,

  3. • no Hɪ depletion in the star formation-enhanced spirals in mixed pairs is found, and

  4. • the high mass (M ≥ 10 M⊙) star formation rate (SFR) in paired Sc spirals is higher than that of the isolated Sc’s by a factor ~ 2 – 3.

Type
Part 2. Properties of Small Groups
Information
International Astronomical Union Colloquium , Volume 174: Small Galaxy Groups , 2000 , pp. 203 - 204
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Faber, S.M., Gallagher, J.S. 1979, ARA&A, 17, 135.Google Scholar
Hernández Toledo, H.M., Dultzin-Hacyan, D., González, J.J., and Sulentic, J.W. 1999, AJ, 118, 108.Google Scholar
Karachentseva, V.E., 1973, Comm. Spec. Ap. Obs. USSR, 8, 1.Google Scholar
Karachentsev, I.D. 1972, Comm. Spec. Ap. Obs. USSR. 7, 1.Google Scholar
Noerdlinger, P.D. 1979, ApJ, 229, 877.CrossRefGoogle Scholar
Rampazzo, R., and Sulentic, J.W. 1992, A&A, 259, 43.Google Scholar
Wiren, S., Zheng, J., Valtonen, M.J., Chemin, A.D. 1996, AJ, 111 160.Google Scholar