Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/vscience/schedule/2014Spring/DenevatagP2860.pdf Дата изменения: Fri Sep 6 19:44:27 2013 Дата индексирования: Sat Mar 1 01:02:01 2014 Кодировка: Поисковые слова: arp 220

Proposal Identification No.:

P2860 Arecibo Observatory

Date Received: 2013-Aug-30 20:51:06 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2013. 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 Pulsars Galactic 55.5 0 1.5 h over 500 GB

Searching for Millisecond Pulsars in Low-Latitude Fermi Unidentified Sources

We propose to search for pulsars in fourteen Fermi unidentified sources close to the Galactic plane (|b|<4 degrees). Such searches have been extremely successful at high Galactic latitudes and low frequencies (327 - 820 MHz). The denser ionized gas environment in the Galactic plane necessitates using higher frequencies in order to minimize scattering and dispersion broadening. We plan to search these sources at 1400 MHz. The benefits of potential discoveries include tests of theories of gravity via timing of binary pulsars, facilitating gravitational wave detection through expanding the set of ob jects included in pulsar timing arrays, and studying the pulsar emission mechanism at various energies. Outreach Abstract: The Fermi spacecraft has detected many ob jects that emit a type of light invisible to the human eye: gamma rays. But it often happens that different types of stars look the same in gamma rays while they look different in other types of light, like radio waves. Using the Arecibo telescope, we want to identify the type of fourteen gamma-ray sources found by Fermi, and specifically to determine whether they are pulsars, a type of star that spins very fast (up to hundreds of times per second) and acts like a lighthouse, giving off a pulse on each rotation. Observing the radio and gamma-ray pulses of Fermi sources that are identified as pulsars helps us learn about how these stars generate the different types of light they emit. These observations will also help us test Einstein's theory of relativity and maybe even detect gravitational waves, ripples in space and time caused by massive ob jects like stars and black holes orbiting closely around each other.

Name Julia Deneva Fernando Camilo

Institution Naval Research Laboratory Arecibo Observatory

E-mail julia.deneva@gmail.com fcamilo@usra.edu

Phone 607-592-5443 787-878-2612, x361

Student no no

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Additional Authors
E. Ferrara (GSFC, elizabeth.c.ferrara@nasa.gov), S. Ransom (NRAO, sransom@nrao.edu), P. Ray (NRL, paul.ray@nrl.navy.mil), M. Kerr (KIPAC, matthew.kerr@gmail.com)

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 0500 ­ 0750 1810 ­ 2100 ­ ­

Days Needed at This Interval 6 15

Time Constraints (Must Be Justified in the Prop osal Text) Anticenter: 3 sessions of 2.75 h each 3 sessions of 2.5 h each Inner Galaxy: 9 sessions of 2.75 h each 6 sessions of 2.5 h each If sessions lengths are scheduled as requested, preferably there will be no more than one session on any given day, and also not on days when PALFA/ZOA is scheduled for 2-3h sessions. This will avoid contention for space on the Mock partitions and use of the machines running the data conversion pipeline 2


that converts Mock data from 16-bit to 4-bit PSRFITS after each PALFA/ZOA session and that will also be used to convert data from this pro ject.

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

Sp ecial Equipment or setup:

none

Section IV - RFI Considerations Frequency Ranges Planned
1225 - 1525 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
Source Name Ra(hh:mm:ss.s) Dec(dd:mm:ss.s) RiseTime TransitTime SetTime P7R40812 05:39:21.0 35:56:02.0 05:00:09 05:40:17 06:20:24 P7R40856A 06:05:56.0 20:39:39.0 04:43:43 06:06:45 07:29:48 P7R40893 06:19:36.0 22:42:14.0 04:58:19 06:20:26 07:42:32 P7R40932 06:42:59.0 09:01:16.0 05:32:17 06:43:44 07:55:11 P7R42942 18:52:51.0 01:58:16.0 18:08:53 18:53:34 19:38:15 P7R42955 18:57:16.0 1:00:04.0 18:19:54 18:57:59 19:36:05 P7R42958A 18:58:06.0 01:28:12.0 18:17:21 18:58:49 19:40:17 P7R42984 19:06:36.0 07:20:20.0 18:00:07 19:07:17 20:14:27 P7R43038 19:25:37.0 17:26:49.0 18:03:31 19:26:15 20:49:00 P7R43069 19:43:53.0 25:17:53.0 18:25:01 19:44:29 21:03:57 P7R43083 19:49:15.0 24:34:23.0 18:29:30 19:49:51 21:10:13 P7R43136 20:04:25.0 33:38:53.0 19:09:43 20:04:59 21:00:14 P7R43175 20:17:54.0 36:27:32.0 19:43:49 20:18:27 20:53:05 P7R43217 20:35:01.0 36:34:51.0 20:02:19 20:35:35 21:08:50

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