Separating M33 Red Giants from Foreground MW Dwarfs

Details Separating M33 Red Giants from Foreground MW Dwarfs Separating M33 Red Giants from Foreground MW Dwarfs

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..374..283t&link_type=abstract

From Stars to Galaxies: Building the Pieces to Build Up the Universe. ASP Conference Series, Vol. 374, proceedings of the confer

Computer Science

Scientific paper

Our goal is to reliably separate foreground Milky Way dwarfs from M33 red giants via photometry in order to study M33's stellar populations (thin disk, thick disk and/or halo). Our technique is based on the gravity sensitivity of the MgI triplet lines and MgH absorption band at λ≈5100 Å in stars with F to K spectral types. The strengths of these lines are quantified photometrically using the narrow-band DDO51 filter. The (V-I) vs (DDO51-V) colors essentially map onto the theoretical temperature-gravity plane, allowing for clean separation between dwarfs and giants of the same temperature for stars with 1⪉(V-I)⪉2. Using the the KPNO 4m telescope and MOSAIC camera, we have obtained photometry for four fields in M33, extending to ˜1°. M33's distance of 794 kpc tep{mjt_mifilt:trgb} and exponential disk scale length of 1.4 kpc tep{mjt_ferg:disk} suggest that the ˜800 candidate M33 stars we observe beyond 0.67° are probably halo/thick disk stars. Our data are also being used to select targets in our spectroscopic companion work.

Affiliated with

Also associated with

No associations

Rating

Separating M33 Red Giants from Foreground MW Dwarfs does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Separating M33 Red Giants from Foreground MW Dwarfs, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Separating M33 Red Giants from Foreground MW Dwarfs will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1108884