1 COS Science Team Meeting October 26, 2007 Baltimore, MD

2 Agenda 9:00 – 9:10: Welcome (Mike Hauser) 9:10 – 9:20: Introduction (Cynthia Froning) 9:20 – 9:40: COS status and schedule (Jim Green) 9:40 – 9:50: STScI resources and timeline (Alessandra Aloisi) 9:50 – 10:10: COS status at STScI (Tony Keyes) 10:10 – 10:30: STScI SMOV planning (Carl Biagetti) 10:30 – 11:00: Coffee break 11:00 – 11:20: Phase II preparation with APT (Karla Peterson) 11:20 – 11:40: COS ETC and BOP (Scott Friedman) 11:40 – 12:00: Life cycle of a Phase II proposal (Denise Taylor) 12:00 – 12:20: TA strategies (Dave Soderblum) 12:40 – 1:00: How to examine/extract COS data with CEDAR (Stephane Beland)

3 Agenda II 1:00 – 2:00: Lunch 2:00 – 2:15: Q&A session with STScI Director (Matt Mountain) 2:15 – 3:20: COS GTO target list 2:15 – 2:20: Overview (Froning) 2:20 – 2:32: IGM (Shull) 2:32 – 2:39: Warm ISM and HVCs (Savage) 2:39 – 2:46: Cold ISM (Snow) 2:46 – 2:53: Galaxies (Leitherer) 2:53 – 2:58: 1 Zw 18 (Heap) 2:58 – 3:05: Cool stars and coronae (Linsky) 3:05 – 3:12: Solar system (Spencer) 3:12 –3:19: XRBs (Froning) 3:20 –3:30: GTO Policies (Neill Reid) 3:30 – 4:00: Coffee break 4:00 – 4:15: Parallels with COS (Ken Sembach) 4:15 – 4:30: COS ERO program (Cynthia Froning) 4:30 – 5:30: Executive session

4 COS GTO Target List

5 GTO Overview A full suite of 551 orbits have been submitted (4 have already been used for ACS observations) A healthy variety of targets, science cases: –IGM (Diffuse IGM, Galaxy interactions, He II G-P, Great Wall tomography) –Star-forming galaxies in the local universe –Warm-hot ISM in HVCs and the LISM (sightlines to AGN, GC stars, WDs) –Cold ISM (translucent and molecular clouds) –Brown dwarfs, cool stars, and coronae –X-ray binaries –Transiting planets –Solar system (atmosphere and aurorae on Io, Callisto, Pluto, comets, KBOs)

6 ProgramOrbits IGM253 Star-forming galaxies20 Warm-hot ISM61 Cold ISM65 Cool stars60 Planetary transits20 XRBs26 Solar system46 Target List Breakdown

7 Proposed COS Observations of X-ray Binaries Cynthia Froning

8 Quiescent X-ray Transients Black hole (BH) or neutron star (NS) accretors with late-type companions Undergo disk outburst on decade timescales Cosmic origins implications: –Study accretion theory up close: outflows (  AGN theory), irradiation (ADAFs), structure, quiescent structure –Nuclear processing effects (CNO), possibly dependant on type of accretor –Li production sites? [C/H] = -1.5 Solar

9 UV Spectroscopy STIS spectra mostly limited to NUV Need COS to get FUV and key lines (CIV, SiIV, NV) UV SED key indicator of disk structure McClintock & Remillard 2000 ApJ, 531, 956 McClintock et al ApJ, 593, 435

10 Targets XTE J A Nova Muscae Select 3-4 interesting targets for GTO observations XTE J : BH system; low extinction; outburst spectrum showed CNO processing A : BH binary; NIR spectrum shows low C Cen X-4: NS binary; STIS spectrum bluer than A (GO proposal) G140L spectra, continuum S/N ≥5 in 5 orbits (per resl), higher in lines Observing Plan: 5-6 orbits ea. G140L, STIS G230L.  26 orbits total Contemporaneous ground-based optical spectroscopy; possibly also X- ray data.

11 ERO Targets Cynthia Froning

12 ERO Selection Process EROs are chosen to highlight the capabilities of the renewed Hubble. They are intended to result in a press release. Targets should be: –Visually compelling –Illustrate new capabilities of facility and instrument –Have scientific content –Provide data for publishable science (but note position on bottom of list) ERO selection is done by GSFC, STScI, and instrument scientists. A broad list of appropriate targets is developed. The list is then sent to NASA HQ, which will take an active role in down-selecting to the final targets

13 ERO Timeline The selection of a list of EROs is being made now Desirability and feasibility being evaluated based on several criteria –Seasonal availability (Fall 2008) –Ease of data acquisition –Use by previous instruments as EROs –Need to look better than previous work –Potential for coordination with multiple instruments List should be finalized around February 2008

14 COS Specifics “Suggestions” from HQ: –One COS ERO should highlight imaging capability –A solar system target would be good How to achieve “visually compelling” with a spectrograph? –Spectra plus illustrations (Mrk 817) –Spectra plus imaging (Nebulae, IC691, Pluto) –Multi-instrument pointings –Targets of public interest (transiting planet) –Targets that could not be observed before (SS 433)

15 ERO Web Pages COS targets: – –Password-protected: enter username “xxxx” and password “xxxx” WFC3 target lists: – – –These are also password-protected

16 Example Presentations