* Astronomy

Title: Local Tadpole Galaxies
Authors: Debra Meloy Elmegreen (1), Bruce G. Elmegreen (2), Jorge Sanchez Almeida (3), Casiana Munoz-Tunon (3), Joseph Putko (1,4), Janosz Dewberry (1) ((1) Vassar College, (2) IBM Research, (3) Instituto de Astrofisica de Canarias, (4) Middlebury College)

Tadpole galaxies have a giant star-forming region at the end of an elongated intensity distribution. Here we use SDSS data to determine the ages, masses, and surface densities of the heads and tails in 14 local tadpoles selected from the Kiso and Michigan surveys of UV-bright galaxies, and we compare them to tadpoles previously studied in the Hubble Ultra Deep Field. The young stellar mass in the head scales linearly with restframe galaxy luminosity, ranging from ~10^5 solar masses at galaxy absolute magnitude U=-13 mag to 10^9 solar masses at U=-20 mag. The corresponding head surface density increases from several solar masses pc^{-2} locally to 10-100 solar masses pc^{-2} at high redshift, and the star formation rate per unit area in the head increases from ~0.01 solar masses yr^{-1} kpc^{-2} locally to ~1 solar masses yr^{-1} kpc^{-2} at high z. These local values are normal for star-forming regions, and the increases with redshift are consistent with other cosmological star formation rates, most likely reflecting an increase in gas abundance. The tails in the local sample look like bulge-free galaxy disks. Their photometric ages decrease from several Gyr to several hundred Myr with increasing z, and their surface densities are more constant than the surface densities of the heads. The far outer intensity profiles in the local sample are symmetric and exponential. We suggest that most local tadpoles are bulge-free galaxy disks with lopsided star formation, perhaps from environmental effects such as ram pressure or disk impacts, or from a Jeans length comparable to half the disk size.

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