Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/vscience/schedule/2013Fall/DemoresttagP2818.pdf Дата изменения: Wed Mar 6 01:08:15 2013 Дата индексирования: Sat Mar 1 01:01:37 2014 Кодировка: Поисковые слова: п п п п п п п п п п п п

Proposal Identification No.:

P2818 Arecibo Observatory

Date Received: 2013-Mar-01 17:50:20 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Mar 1 2013. This proposal has not been submitted before. Proposal Type: General 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: Regular Pulsars Galactic 18 0 0 0 1.5 hours less than 100 GB

Expanding the NANOGrav Pulsar Timing Array

Direct detection of gravitational waves (GW) is a ma jor goal in experimental physics and will open an entirely new astronomical spectrum. Precision pulsar timing stands an excellent chance of being the first method to accomplish this feat. Combining data from many ob jects into a Pulsar Timing Array (PTA) makes GW detection possible. Increasing the number of pulsars in the array improves sensitivity, and over the past few years we have doubled our source list by including newly discovered pulsars. New instrumentation for pulsar timing (PUPPI) now provides an order of magnitude more bandwidth than previously available. In this proposal, we request time to revisit several older pulsar discoveries that with previous instrumentation were either too faint or unreliably detected (due to scintillation) to be useful. When observed with PUPPI we expect several of these sources may now be useful additions to the NANOGrav pro ject. Outreach Abstract: Our pro ject aims to detect gravitational waves ­ tiny ripples in space-time predicted by Einstein's theory of general relativity. Although they were predicted nearly 100 years ago, because they are so weak these waves have still never been detected directly. In our pro ject, we use millisecond pulsars ­ rapidly spinning neutron stars ­ as a set of clocks distributed throughout our galaxy. We measure the clocks rates by receiving their radio pulses with the Arecibo telescope. Gravitational waves will cause small changes in the apparent spin rate of each pulsar. If we can successfully detect them, these waves will give us information about the number and properties of black holes that exist in our universe.

Name Paul B Demorest David J Nice

Institution NRAO Lafayette College

E-mail pdemores@nrao.edu niced@lafayette.edu

Phone 434-244-6838 610-330-5204

Student no no

1


Additional Authors
Ingrid Stairs stairs@astro.ubc.ca Scott Ransom sransom@nrao.edu Zaven Arzoumanian zaven.arzoumanian@nasa.gov Jim Cordes cordes@astro.cornell.edu Robert Ferdman rferdman@physics.mcgill.ca Glenn Jones glenn.caltech@gmail.com Maura McLaughlin maura.mclaughlin@mail.wvu.edu Timothy Pennucci (grad) ttp4tx@virginia.edu Joseph Swiggum (grad) swiggumj@gmail.com Weiwei Zhu zhuww@phas.ubc.ca NANOGrav Collaboration nano-time@nanograv.org Emmanuel Fonseca (grad) efonseca@phas.ubc.ca Kevin Stovall (grad) kstovall@phys.utb.edu

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 not needed.

Begin ­ End Interval­Interval 14:30 ­ 17:30 19:00 ­ 21:00 18:00 ­ 19:30 21:30 ­ 23:00

Days Needed at This Interval 2 2 2 2

Time Constraints (Must Be Justified in the Prop osal Text) J1453+1902 and J1709+2313 can be observed together in a 3-hour session, beginning near 14.5h LST J2019+2425 and J2033+17 can be observed together in a 3-hour session, beginning near 19h LST. 2


J1911+1347 and J2229+2643 can each be observed in individual 1.5-hour sessions. The two sessions for each source should be spaced apart by at least two weeks. If possible, please schedule all sessions before the September 1 proposal deadline. Aside from the above constraints, scheduling of the individual sessions do not need any special coordination with each other or with the other monthly NANOGrav observations.

Section I I I - Instruments Needed
430 G L-wide S-low

Atmospheric Observation Instruments:

Sp ecial Equipment or setup: PUPPI

Section IV - RFI Considerations Frequency Ranges Planned
420 - 440 1150 - 1800 1700 - 2400

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 RA Dec RiseLST SetLST J1453+1902 14:53:45.7 19:02:12.2 13:31 16:17 J1709+2313 17:09:05.7 23:13:27.8 15:47 18:31 J1911+1347 19:11:55.2 13:47:34.4 17:52 20:32 J2019+2425 20:19:31.9 24:25:15.3 18:59 21:40 J2033+17 20:33:21.0 17:36:00.0 19:11 21:56 J2229+2643 22:29:50.8 26:43:57.7 21:13 23:47

3