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Proposal Identification No.:

A2763 Arecibo Observatory

Date Received: 2012-Sep-02 19:16:08 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2012. This proposal has been submitted before. The previous proposal number is A2059 and A2124. Proposal Type: General Category: Sub-Category: Observation Category: Time Requested this semester: Hours Next Semester: Hours already used for this pro ject: Additional Hours required to complete pro ject: Minimum Useful Time: Expected Data Storage: Prop osal Title: ABSTRACT: Commensal Astronomy Spectroscopy Galactic 1326 (w/ GALFACTS and AGES) 411 (w/ AGES) approx 3000 w/ GALFACTS and AGES

less than 100 GB

The Galactic Arecibo L-Band Feed Array HI (GALFA-HI) Survey

Hydrogen is the basic baryonic building block of galaxies. Gas flows into the dark matter potential well of a galaxy, condenses in the disk in atomic form, and subsequently forms molecular material and then stars. Several crucial questions remain open as to how this process occurs and how stars subsequently shape the interstellar medium (ISM). We began the GALFA-HI Survey (originally called the Turn on GALFA Survey (TOGS)) in 2005 to map the kinematic and spatial distribution of our Galaxy's neutral hydrogen and address these questions. GALFA-HI optimizes on Arecibo's new commensal capabilities and observes with ALFALFA, AGES, and GALFACTS. It is commensally surveying HI over 13,000 sq. deg of the sky with a high angular and spectral resolution (4' and 0.18 km/s) and wide bandwidth (+/- 700 km/s). This proposal is to complete the GALFA-HI Survey through commensal observations with AGES and GALFACTS and study the relationship of Galactic HI to stars and other Galactic components. Outreach Abstract: Galaxies like the Milky Way forms stars from hydrogen gas. The GALFA-HI survey studies how this gas gets into the Milky Way to form new stars. It also looks at how stars influence the surrounding gas when they end their lives.

Name Mary E Putman Snezana Stanimirovic

Institution Columbia University UW-Madison

E-mail mputman@astro.columbia.edu sstanimi@astro.wisc.edu

Phone 2128546831

Student no no

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Additional Authors
Josh Peek (goldston@gmail.com) Carl Heiles (heiles@astro.berkeley.edu) Eric Korpela (korpela@ssl.berkeley.edu) Steven Gibson (steven.gibson@wku.edu) Destry Saul (student; destrys@gmail.com) Min-Young Lee (student; lee@astro.wisc.edu) Jana Grcevich (janagrc@gmail.com) Kevin Douglas (kevindouglasphd@gmail.com)

This work is part of a PhD thesis.

Remote Observing Request

Observer will travel to AO Remote Observing X In Absentia (instructions to operator)

Section I I - Time Request
The following times are in LST. For these observations night-time is .

Begin ­ End Interval­Interval ­ ­ ­ ­

Days Needed at This Interval

Time Constraints (Must Be Justified in the Prop osal Text) These observations are all commensal with GALFACTS and AGES. Approximately 3% is added to their time to complete our calibrations.

Next Semester Time Request

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Begin ­ End Interval­Interval ­ ­ ­ ­

Days Needed at This Interval

Time Constraints (Must Be Justified in the Prop osal Text)

Section I I I - Instruments Needed
ALFA Atmospheric Observation Instruments:

Sp ecial Equipment or setup:

none

Section IV - RFI Considerations Frequency Ranges Planned

This proposal requires coordination with Punta Salinas radar within the band 1222-1381 MHz.. This proposal requires coordination with GPS L3 at 1381 MHz.

Section V - Observing List Target List

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