eCite Digital Repository

Stellar Populations at the Center of IC 1613


Cole, AA and Tolstoy, E and Gallagher, JS and Hoessel, JG and Mould, JR and Holtzman, JA and Saha, A and Ballester, GE and Burrows, CJ and Clarke, JT and Crisp, D and Griffiths, RE and Grillmar, CJ and Hester, JJ and Krist, JE and Meadows, V and Scowen, PA and Stapelfeldt, KR and Trauger, JT and Watson, AM and Westphal, JR, Stellar Populations at the Center of IC 1613, The Astronomical Journal, 118, (4) pp. 1657-1670. ISSN 0004-6256 (1999) [Refereed Article]

DOI: doi:10.1086/301042


We have observed the center of the Local Group dwarf irregular galaxy IC 1613 with the WFPC2 aboard the Hubble Space Telescope in the F439W, F555W, and F814W filters. We analyze the resulting color-magnitude diagrams (CMDs) using the main-sequence and giant-branch luminosity functions and comparisons with theoretical stellar models to derive a preliminary star formation history for this galaxy. We find a dominant old stellar population (age ≈ 7 Gyr), identifiable by the strong red giant branch (RGB) and red clump populations. From the (V - I) color of the RGB, we estimate a mean metallicity of the intermediate-age stellar population [Fe/H] = -1.38 ± 0.31. We confirm a distance of 715 ± 40 kpc using the I magnitude of the RGB tip. The main-sequence luminosity function down to I ≈ 25 provides evidence for a roughly constant star formation rate (SFR) of approximately 3.5 × 10 -4 M ⊙ yr -1 across the WFPC2 field of view (0.22 kpc 2 ) during the past 250-350 Myr. Structure in the blue loop luminosity function implies that the SFR was ≈ 50% higher 400-900 Myr ago than today. The mean heavy-element abundance of these young stars is around one-tenth solar. The best explanation for a red spur on the main sequence at I ≈ 24.7 is the blue horizontal branch component of a very old stellar population at the center of IC 1613. We have also imaged a broader area of IC 1613 using the 3.5 m WIYN telescope under excellent seeing conditions. The WIYN CMD reveals a prominent sequence of asymptotic giant branch stars and red supergiants that is less prominent in the WFPC2 CMD because of the smaller field of view. The asymptotic giant branch star luminosity function is consistent with a period of continuous star formation over at least the age range 2-10 Gyr. We present an approximate age-metallicity relation for IC 1613, which appears to be similar to that of the Small Magellanic Cloud. We compare the Hess diagram of IC 1613 with similar data for three other Local Group dwarf galaxies and find that IC 1613 most closely resembles the nearby, transition-type dwarf galaxy Pegasus (DDO 216).

Item Details

Item Type:Refereed Article
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Galactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Cole, AA (Associate Professor Andrew Cole)
ID Code:45317
Year Published:1999
Web of Science® Times Cited:73
Deposited By:Physics
Deposited On:2007-07-10
Last Modified:2007-07-10

Repository Staff Only: item control page