Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/vscience/schedule/2014Fall/HeilestagA2898.pdf Дата изменения: Thu Mar 6 22:59:04 2014 Дата индексирования: Mon Apr 11 15:29:04 2016 Кодировка: Поисковые слова: http astrokuban.info astrokuban

Proposal Identification No.:

A2898 Arecibo Observatory

Date Received: 2014-Feb-26 20:44:24 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Mar 1 2014. This proposal has not been submitted before. Proposal Type: General Category: Observation Category: Time Requested this 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: Regular Astronomy Galactic 297 0 1.5 hours less than 100 GB

Tracing Dark Molecular Gas with OH Emission

There is great interest these days in the transition between atomic and molecular interstellar gas, which should represent the very initial stages of star formation. Molecular gas means Molecular Hydrogen (H2)--Hydrogen dominates the elemental abundance. While H2 is normally traced by CO emission, there exists Dark Molecular Gas (DMG), which contains H2 but is not traced by CO emission. This gas is probably in the transition state. It is best traced by OH, HCO+, and CO in absorption, and an unknown degree in emission. This proposal explores DMG by mapping OH in regions where DMG is known to exist from these tracers in absorption. Outreach Abstract: There is great interest these days in the transition between atomic and molecular interstellar gas, because it should represent the very initial stages of star formation. Molecular gas means Molecular Hydrogen (H2), because Hydrogen overwhelmingly dominates the elemental abundance of cosmic ob jects such as interstellar gas and stars. While H2 is normally traced by CO emission, there exists so-called Dark Molecular Gas (DMG), which contains H2 but is not traced by CO emission. DMG is probably in the atomic-to-molecular transition state. DMG is best traced by OH, HCO+, and CO in absorption against background radio sources, and also to an unknown degree in emission. This proposal explores DMG by mapping OH in regions where DMG is known to exist from these tracers in absorption.

Name Carl Heiles Steven Gibson

Institution university of california, berkeley Western Kentucky University

E-mail heiles@astro.berkeley.edu Steven Gibson

Phone 510 280 8099 270-745-3019

Student no no

1


Additional Authors
Bon-Chul Koo , Joanne.Dawson@csiro.au, Di Li , heiles@astro.berkeley.edu, anne.green@sydney.edu.au, Naomi McClure-Griffiths , Steven Gibson , Richard L. PLAMBECK , cmurray@astro.wisc.edu, ktkim@kasi.re.kr, John Dickey , tim.robishaw@nrc-cnrc.gc.ca, L. Bronfman

This work is not part of a thesis.

Remote Observing Request

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

Section I I - Time Request
The following times are in LST. For these observations night-time is not needed.

Begin ­ End Interval­Interval 04:12 ­ 06:51 07:22 ­ 10:00 21:32 ­ 00:16 ­

Days Needed at This Interval 36 36 36

Time Constraints (Must Be Justified in the Prop osal Text) no constraints, except that the sun should not be within 20 degrees of the ob ject being observed.

Section I I I - Instruments Needed
L-wide Atmospheric Observation Instruments: 2


Sp ecial Equipment or setup: We will use the interim correlator, which is ideal for our purposes.

Section IV - RFI Considerations Frequency Ranges Planned
1420.4 MHz 1665-1667 MHz 1720 MHz

Section V - Observing List Target List
ob ject,,,........,,,,,,RA............Dec.........rise-set B0528+134...05:30:46.41...13:31:55.1...04:12.to.06:51 3C207...........08:40:47.59...13:12:23.6...07:22.to.10:00 3C454.3........22:53:57.71...16:08:53.4...21:32.to.00:17

3