Time Scales Of Bulge Formation In Nearby Galaxies

Time Scales Of Bulge Formation In Nearby Galaxies Traditionally, bulges are thought to fit well into galaxy formation models of hierarchical merging. However, it is now becoming well established that many bulges formed through internal, secular evolution of the disk rather than through mergers. We call these objects pseudobulges. Much is still unknown about pseudobulges, the most pressing questions being: How, exactly, do they build up their mass? How long does it take? And, how many exist? We are after an answer to these questions. If pseudobulges form and evolve over longer periods than the time between mergers, then a significant population of pseudobulges is hard to explain within current galaxy formation theories. A pseudobulge indicates that a galaxy has most likely not undergone a major merger since the formation of the disk. The ages of pseudobulges give us an estimate for the time scale of this quiescent evolution. We propose to use 24 orbits of HST time to complete UBVIH imaging on a sample of 33 nearby galaxies that we have observed with Spitzer in the mid-IR. These data will be used to measure spatially resolved stellar population parameters (mean stellar age, metallicity, and star formation history); comparing ages to star formation rates allows us to accurately constrain the time scale of pseudobulge formation. Our sample of bulges includes both pseudo- and classical bulges, and evenly samples barred and unbarred galaxies. Most of our sample is imaged, 13 have complete UBVIH coverage; we merely ask to complete missing observations so that we may construct a uniform sample for studying bulge formation. We also wish to compare the stellar population parameters to a variety of bulge and global galaxy properties including star formation rates, dynamics, internal bulge morphology, structure from bulge-disk decompositions, and gas content. Much of this data set is already or is being assembled. This will allow us to derive methods of pseudobulge identification that can be used to accurately count pseudobulges in large surveys. Aside from our own science goals, we will present this broad set of data to the community. Thus, we waive proprietary periods for all observations.

We wish to obtain surface photometry in each band. We originally wanted ACS/WFC for B,V,I and ACS/HRC for U. However, we are lucky that all of our science objectives can be achieved with WFPC2, centering galaxies on the PC chip. We are primarily interested in the PC chip, thus the WF4 anamoly will not affect us. In 2-gyro mode WFPC2 can obtain signal-to-noise per pixel of S/N ~ 15-20 for an 18th V magnitude extended source with exposure times of t_{exp}=800s for F450W, t_{exp}=400s for F555W and t_{exp}=250s for F814W. We will CR-SPLIT each image to reduce the effect of cosmic rays. And we can reach S/N~20 for all our galaxies with a 250 second exposure, CR-SPLIT with NICMOS 2 F160W is adequate to reach deep magnitudes. Each galaxy will be centered in the frame. The proposed observations are heavily weighted toward F336W observations. F336W is the least observed filter in the archive for our sample, and requires, by far, the longest integration times. However, F336W is necessary to determine stellar population quantities with accuracy. Previous groups have had mixed results with HST U band data. To insure a succesfull program we only target nearby galaxies, and expose longer. Using ACS/HRC with F336W we set exposure times based on the surface brightness profiles, increasing exposure times for fainter galaxies. We require a minimum of S/N~3 at ~9 arcsec, this allows us to overlap a few resolution elements in a ground based U band image, for constructing a composite space plus ground profile. To correct for possible saturation we plan to add a 60s exposure in F814W at the beginning of the observation sequence. In the event of unpacked orbits, we use the autoamtic orbit packing option to increase exposure times. Calculation of the surface photometry will be done with software from Bender & Moellenhoff (1987). The required software is well developed, and the PI (Fisher) is experienced at using this software. We will obtain wide-field ground-based data for each galaxy giving a greater dynamic range to color and structural profiles. Most of these observation have already been made at the McDonald 0.8-m. The overlap between ACS/WFC and ground-based telescopes provides confirmation for derived quantities. We are confident that the program will be completed and submitted for publication within one year after the completion of HST observations. 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