AAS 197, January 2001
Session 76. Galaxy Evolution I
Display, Wednesday, January 10, 2001, 9:30am-7:00pm, Exhibit Hall

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[76.03] The MALIGN Survey Overview and the IR Luminosity Function by Morphological Type

J.P. Huchra (CfA), M.A. Pahre (CfA), C.S. Kochanek (CfA), E.E. Falco (SAO), J. Mader (CfA), T. Jarrett (IPAC), T. Chester (IPAC), S. Schneider (UMASS/Amherst)

The MALIGN survey (Masses And Luminosities of Infrared Galaxies Nearby) is an investigation into the dynamics and other global properties of galaxies in the local universe. Two samples of galaxies selected from the 2MASS survey have been defined: (1) all galaxies (> 4000) with apparent isophotal magnitudes 7 \leq K20 \leq 11.25~mag, Galactic latitude |b| \geq 20\circ, and Declination \delta \geq 11.5\circ; and (2) a smaller, randomly-selected subsample of ~500 galaxies at 10.5 \leq K20 \leq 11.25~mag. The first sample has complete redshifts, thus providing the luminosities for the computation of the luminosity function, and the entire sample has been classified morphologically from the digitized sky survey. The second sample is being studied more intensively, by obtaining long-slit, moderate dispersion absorption-line and emission-line spectroscopy, in order to measure rotation curves and velocity dispersion profiles. These data are supplemented by optical and near-infrared surface photometry, in order to separate the disk and bulge components.

This paper presents an overview of the MALIGN survey for both samples. The near-infrared K-band luminosity function is constructed from the 4206 galaxy sample, and is broken into late- and early-type components. The early- and late-type LFs shows little difference in their relatively flat faint end slopes, but the late-type LF has a characteristic luminosity that is ~0.5~mag fainter in the K-band.

The 2MASS Survey is supported by NASA, the NSF, the Air Force and the Navy.

If you would like more information about this abstract, please follow the link to http://cfa-www.harvard.edu/~mpahre/malign/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: jhuchra@cfa.harvard.edu

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