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Proposal Identification No.:

A2943 Arecibo Observatory

Date Received: 2014-Aug-31 20:47:39 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 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 67.5 21.5 0 1 hour 100-500 GB

OH Survey along GOT C+ Sightlines

Growing observational evidence supports the existence of so-called "CO-dark molecular gas (DMG)", which comprises a substantial fraction of the ISM that is not completely traced by either CO or HI emission. Previous studies have showed that C+, OH and HCO+ do reliably trace the DMG even with its harsh UV environment. The relation of N(OH) and N(HCO+) is exactly 0.03 with small errorbars (Lucas and Liszt 1996). The Galactic observations of TeraHertz C+ (GOT C+), a Herschel Key Pro ject, has surveyed 454 C+ 158um spectra toward the Galactic plane. We propose to observe OH spectra along those GOT C+ sightlines to compare the relation between N(C+) and N(OH) in tracing DMG. The proposed Arecibo OH survey will potentially help quantify DMG by establishing the relation between key oxygen and Carbon species in the intermediate extinction ISM regime. Outreach Abstract: Interstellar medium (ISM) is cradle of star formation. Emission of atomic hydrogen and carbon monoxide are main tracers of ISM. An additional phase which called dark molecular gas (DMG) can't be revealed by atomic hydrogen or carbon monoxide emission. Ionized carbon, hydroxyl and formylium are main tracers of DMG, but participate in different chemical reactions. However, the relation between column density of hydroxyl and ionized carbon are found to be exactly linear. The relation between column density of ionized carbon and hydroxyl has not been investigated yet. Motivated by this, we propose to observe OH towards 59 sightlines which have ionized carbon spectra already. It will greatly improve our understanding of ISM phases and result in a new view of stellar evolution.

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Name Ningyu Tang

Carl Heiles

Institution National Astronomical Observatories, Chinese Academy of Sciences University of California, Berkeley

E-mail astrotomny@gmail.com

Phone 08618811731183

Student G

heiles@astro.berkeley.edu

(510)6424510

no

Additional Authors
Di Li Paul F. Goldsmith Jorge Pineda Naomi McClure-Griffiths

This work is part of a PhD thesis.

Remote Observing Request

X

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

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

Begin ­ End Interval­Interval 18:00 ­ 21:00 04:30 ­ 07:30 ­ ­

Days Needed at This Interval 20 5

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

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

Sp ecial Equipment or setup:

none

Section IV - RFI Considerations Frequency Ranges Planned
1612 1665-1667 1720

Section V - Observing List Target List
G032.6+0.0 18:50:44.8 -0:20:13.4 G032.6+0.5 18:48:58.0 -0:06:32.6 G033.8-0.5 18:54:51.4 0:34:15.8 G035.1+0.0 18:55:24.3 1:56:06.6 G035.1+0.5 18:53:37.5 2:09:47.6 G036.4+0.0 18:57:44.3 3:04:15.7 G036.4-1.0 19:01:18.0 2:36:50.5 G038.9-0.5 19:04:12.4 5:06:45.2 G041.5+0.0 19:07:08.3 7:36:36.5 G041.5-0.5 19:08:55.8 7:22:47.6 G041.5-1.0 19:10:43.1 7:08:57.1 G042.8+0.0 19:09:30.9 8:44:35.5 G042.8+1.0 19:05:55.2 9:12:12.5 G044.0+0.0 19:11:54.4 9:52:31.2 G044.0-1.0 19:15:30.0 9:24:40.8 G045.3+0.0 19:14:18.8 11:00:22.8 G045.3+1.0 19:10:42.0 11:28:10.2 G046.6-0.5 19:18:32.9 11:54:09.5 G047.9+0.0 19:19:11.2 13:15:53.1 G047.9+0.5 19:17:22.2 13:29:55.0 G047.9+1.0 19:15:32.9 13:43:53.8 G049.1+0.0 19:21:39.4 14:23:30.6 G049.1-1.0 19:25:17.5 13:55:09.7 G050.4+0.0 19:24:09.1 15:31:02.3 G050.4+1.0 19:20:29.1 15:59:19.1 G051.7+0.0 19:26:40.4 16:38:27.6 G051.7-1.0 19:30:20.1 16:09:47.1 G053.0+0.0 19:29:13.5 17:45:46.0 G054.3+0.0 19:31:48.5 18:52:56.8 3


G054.3-0.5 19:33:39.5 18:38:27.3 G056.8+0.0 19:37:05.0 21:06:53.4 G056.8-0.5 19:38:57.0 20:52:11.3 G056.8-1.0 19:40:48.7 20:37:24.6 G058.1+0.0 19:39:46.8 22:13:37.9 G058.1+0.5 19:37:53.8 22:28:22.1 G058.1+1.0 19:36:00.3 22:43:01.4 G060.0+0.0 19:43:54.3 23:53:25.4 G060.0-0.5 19:45:47.9 23:38:25.1 G060.0-1.0 19:47:41.0 23:23:19.7 G064.5+0.0 19:54:06.6 27:47:38.2 G064.5+0.5 19:52:10.0 28:03:03.0 G064.5+1.0 19:50:13.0 28:18:21.6 G069.1+0.0 20:05:04.2 31:38:49.9 G069.1-0.5 20:07:02.9 31:22:42.4 G069.1-1.0 20:09:00.9 31:06:28.0 G073.6+0.0 20:16:58.2 35:26:12.8 G073.6+0.5 20:14:55.8 35:42:56.3 G073.6+1.0 20:12:52.4 35:59:32.0 G168.7-1.0 05:11:30.5 37:48:25.0 G168.7-2.0 05:07:31.1 37:11:42.7 G184.5+0.0 05:56:01.8 25:02:46.4 G184.5+1.0 05:59:51.6 25:32:47.2 G184.5+2.0 06:03:39.7 26:03:54.2 G189.1-1.0 06:02:04.1 20:37:19.4 G189.1-2.0 05:58:27.3 20:05:18.6 G202.6+0.0 06:32:30.5 9:08:51.3 G202.6+1.0 06:36:06.4 9:36:29.9 G202.6+2.0 06:39:38.2 10:06:14.5 G207.2-2.0 06:33:49.5 4:10:54.0

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