Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/vscience/schedule/2014Fall/LitagA2901.pdf Дата изменения: Thu Mar 6 22:59:19 2014 Дата индексирования: Mon Apr 11 13:24:15 2016 Кодировка: Поисковые слова: millennium

Proposal Identification No.:

A2901 Arecibo Observatory

Date Received: 2014-Mar-03 05:50:59 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 21.5 0 0 30 min less than 100 GB

OH Survey of Dark Molecular Gas in the Galactic Plane

Dark Molecular Gas (DMG) is a phase of the interstellar medium that is traced by neither 21-cm emission (HI) nor 3-mm CO emission. In DMG, hydrogen is in molecular (H2) form but carbon (CI, CII) is not, i.e., without CO emission. This situation is possible in regions of modest extinction where H2 self-shielding is operative but the UV flux is sufficient to destroy CO. Heiles and Troland (2003) observed OH absorption along with HI in their Arecibo Millennium survey, showing that OH could trace DMG. The Herschel key program GOTC+ has identified sites of potential DMG based on CII emission (Pineda et al. 2013). Combining the key elements of both influential surveys, we propose an OH survey of DMG candidates identified by GOTC+. Combined with HI, C+, and CO data, the proposed survey could provide a systematic view of the quantity and excitation conditions of DMG. Outreach Abstract: Stars are formed in the interstellar medium (ISM). We have been using emission of atomic hydrogen and carbon monoxide to trace the ma jority of ISM. In recent years, a growing body of evidence suggests the existence of so-called dark molecular gas (DMG), which cannot be revealed by simply looking at HI or CO emission. We propose to observe OH toward 30 candidate sites of DMG. OH is the first interstellar molecule discovered by human and is one of the simplest radical in space. Our proposed study aims to quantify DMG and its physical conditions. These information is critical for understanding the formation of stars.

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Name Di Li

Nannan Yue

Institution National Astronomical Observatories, Chinese Academy of Sciences National Astronomical Observatories, Chinese Academy of Sciences

E-mail ithaca.li@gmail.com

Phone 0861064806305

Student no

yuenannan0907@gmail.com

08618901268939

G

Additional Authors
Carl Heiles Naomi McClure-Griffiths Ningyu Tang

This work is part of a PhD 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 preferred.

Begin ­ End Interval­Interval 6:00 ­ 9:00 18:00 ­ 21:00 ­ ­

Days Needed at This Interval 2 9

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

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no

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

Sp ecial Equipment or setup:

none

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

Section V - Observing List Target List
G032.6+1.0 18h47m11.28s +00d07m08.40s G033.8-1.0 18h56m38.16s +00d20m34.80s G033.8+0.0 18h53m04.56s +00d47m56.76s G035.1+1.0 18h51m50.64s +02d23m27.96s G036.4-0.5 18h59m31.20s +02d50m33.36s G037.7+0.0 19h00m04.56s +04d12m23.76s G037.7+0.5 18h58m17.52s +04d26m05.99s G037.7+1.0 18h56m30.48s +04d39m47.88s G038.9-1.0 19h05m59.28s +04d52m59.16s G038.9+0.0 19h02m25.20s +05d20m30.12s G040.2+0.0 19h04m46.56s +06d28m34.32s G040.2+0.5 19h02m59.04s +06d42m19.80s G040.2+1.0 19h01m11.76s +06d56m03.47s G042.8+0.5 19h07m43.20s +08d58m24.96s G044.0-0.5 19h13m42.24s +09d38m36.96s G045.3+0.5 19h12m30.48s +11d14m17.88s G046.6-1.0 19h20m21.12s +11d40m06.24s G046.6+0.0 19h16m44.40s +12d08m10.68s G049.1-0.5 19h23m28.56s +14d09m21.96s G050.4+0.5 19h22m19.20s +15d45m12.60s G051.7-0.5 19h28m30.48s +16d24m09.36s G053.0+0.5 19h27m22.80s +18d00m06.11s G053.0+1.0 19h25m31.68s +18d14m21.84s G054.3-1.0 19h35m30.24s +18d23m53.88s G055.5+0.0 19h34m25.67s +19d59m59.64s G055.5+0.5 19h32m33.85s +20d14m30.84s 3


G055.5+1.0 19h30m41.52s +20d28m57.72s G189.1+0.0 06h05m47.71s +21d06m49.32s G207.2-1.0 06h37m19.92s +04d40m04.80s G207.2+0.0 06h40m54.00s +05d07m35.04s

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