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ARCSAT ID NUMBER: AS08

DESCRIPTIVE TITLE: Kepler Eclipsing Binaries

PI: Suzanne Hawley

OBSERVER(S): Jim Davenport

UNCERTIFIED/UNTRAINED OBSERVERS: UW AST 581 observing class

COLLABORATORS: Leslie Hebb
 
CONTACT INFORMATION: jrad@astro.washington.edu, slh@astro.washington.edu

NUMBER OF WEEKS REQUESTED: 2

TIME REQUESTED: July 20-26, Sept 14-20

INSTRUMENT: Flarecam

FILTERS: ugriz

COMMENTS: We will be on-site during Sept 18-20

BRIEF SCIENCE JUSTIFICATION: 
This is a continuation of an ongoing UW program to investigate eclipsing binaries discovered with Kepler, in particular to obtain ground-based multi-color photometry during eclipses.


ARCSAT ID NUMBER: AS09

DESCRIPTIVE TITLE: Monitoring H-alpha Variability in Be Stars in Young Clusters

PI: Steven Souza (Williams College)

OBSERVER(S): Steven Souza

UNCERTIFIED/UNTRAINED OBSERVERS: summer research students Hallee Wong (Williams 
	College '18), Aylin Garcia Soto (Wesleyan University '18) 

COLLABORATORS: none
 
CONTACT INFORMATION: Steven Souza; ssouza@williams.edu; 413-441-9892

TIME REQUESTED: My request is for one week total during Q3. My preference is to have
this in the form of one block of 3 days and one of 4 days, from any of the following:
week of 7/13 - 7/19		second half (7/13-15 excluded)
week of 7/20 - 7/26
week of 8/3 - 8/9
week of 8/10 - 8/16		first half (8/13-16 excluded)
week of 8/17 - 8/23
week of 8/31 - 9/6		second half (8/31-9/3 excluded)
week of 9/7 - 9/13		first half (9/10-9/13 excluded)

If scheduling split weeks proves too difficult, I can use any one full week of:
week of 7/20 - 7/26
week of 8/3 - 8/9
week of 8/17 - 8/23

INSTRUMENT: SurveyCam

FILTERS: halpha_6563_50, rc_6450_50

COMMENTS: If time is granted between 7/13 and 8/9, it will provide data for two 
undergraduate students working with me during our summer science research session. 
After the first observable night I would like permission to allow the students to 
operate the system, although I would be present and supervise them at all times.

BRIEF SCIENCE JUSTIFICATION:
In Be stars both continuum and emission lines vary irregularly, but spectroscopic 
monitoring has been undertaken for only a few individual bright stars. A larger sample 
can be reached via narrowband imaging using matched on-band (656nm) and off-band (645nm) 
filters, as we have been doing on the Williams College 0.6-m DFM telescope for the last 
5 years. Our program to monitor early-type emission-line stars is focused on young open 
clusters and associations. To date we have characterized H-alpha and continuum variations 
in 10 Be stars in NGC659 and NGC663, found 4+ new Be stars and ~20 new candidate 
variables, and incidentally refined the orbital period of an eclipsing binary in the 
Cygnus OB2 association.

Observations at ARCSAT, using a camera and filters similar to those we use at Williams, 
are intended to add short periods of good temporal coverage to complement the longer-
term, but sparser, observations at Williams. As an early ARCSAT user I found that data 
obtained using SurveyCam and narrowband filters on loan to ARC from Williams College 
are better than data obtained at Williams. Many of the ~20 clusters in our target list 
can be observed during any of the periods requested.