PHAT M31 Cluster Images

Jan 10, 2014

This password protected site is a modified version of my public M31 site. It contains the information on M31 clusters contained in the public page as well as postage stamps from the PHAT images. The files used for these images came from the PHAT pipeline. Names are from the Andromeda Project and the Revised Bologna Catalog where possible. "hodge09" and "hodge10" names are from Hodge et al. (AJ, 138, 770, 2009) and Hodge et al. (PASP, 122, 745, 2010).

All clusters in the PHAT footprint, found by the AP or others, ordered by magnitude. Only good AP clusters are included.

All clusters ordered by name.

All observed clusters, ordered by RA.

Same, ordered by spectroscopic metallicity.

Clusters intended for Old cluster paper, ordered by name.

Clusters with good cmds, intended for the Old cluster paper, ordered by mass.

All observed clusters, ordered by distance to center of M31.

All clusters in the PHAT footprint recently studied by Lori Beerman, new and previously known, ordered by magnitude. Her masses and ages are shown.

All observed clusters whose spectra show evidence of ionized gas, usually from Halpha.

Stars which have Hectospectra.

Stars which Massey has provided spectral types for.

For each object in these lists, the following are shown:
Each web page contains a list of objects to the left, ordered as stated. The images will appear to the right after clicking. Basic information appears next to the images (type, velocity, V magnitude, comments).  Mass, [Fe/H] and ages are from Caldwell et al. 2009 and a recently accepted AJ paper. Please don't distribute this material till that paper appears in astro-ph. "Type" is explained in the catalog notes (see public link above).

The ground based images come from the Local Group Survey of Massey et al. 2006, AJ, 131, 2478. Magnitudes are not yet rationalized (most are actually V, but some of the smaller, young clusters are F555W, and worse). They are meant to be indicative only. Spectra of the young clusters are in jpg format. Click on the postage stamp for full resolution. The spectra (aside of a few problem cases that are obvious - young clusters with red continua) have been flux calibrated, deredshifted (actually deblueshifted) and dereddened. These plots show only the blue part of the spectrum. The data was smoothed before plotting.