Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/vscience/schedule/2013Spring/DemoresttagP2780.pdf Дата изменения: Tue Sep 11 04:14:21 2012 Дата индексирования: Tue Feb 5 00:05:17 2013 Кодировка: Поисковые слова: south pole

Proposal Identification No.:

P2780 Arecibo Observatory

Date Received: 2012-Sep-04 15:39:41 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2012. 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: Large Pulsars Extragalactic 185 185 680 1500 1.5 hours less than 100 GB

The North American Nanohertz Observatory for Gravitational Waves

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. Long timing baselines (5­10 years) dramatically improve GW sensitivity. Increasing the number of pulsars in the array also improves sensitivity, and the past several years have seen a unexpected number of new millisecond pulsars discovered. New instrumentation for pulsar timing now provides an order of magnitude more bandwidth than previous instruments. In this proposal, we request time to continue and expand our ongoing PTA pro ject over the next year, taking advantage of all these improvements. These results will provide the best GW sensitivity yet achieved, and will significantly constrain the astrophysics of GW sources. 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

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

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 14:00 ­ 01:30 17:05 ­ 22:05 16:55 ­ 20:55 ­

Days Needed at This Interval 9 9 9

Time Constraints (Must Be Justified in the Prop osal Text) The 9 requested epochs for each type of session (A, B or C as described in the proposal) should be scheduled with approximately 20-day spacing. The spacing between different session types (eg, the A-B spacing) is not constrained.

Next Semester Time Request

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Begin ­ End Interval­Interval 14:00 ­ 01:30 17:04 ­ 22:05 16:55 ­ 20:55 ­

Days Needed at This Interval 9 9 9

Time Constraints (Must Be Justified in the Prop osal Text) Same as for first semester.

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

Atmospheric Observation Instruments:

Sp ecial Equipment or setup: PUPPI (primary) ASP (backup; to be discontinued in 1 year)

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
Session A: J1640+2224 16:40:16.7 22:24:08.9 J1713+0747 17:13:49.5 07:47:37.5 J1853+1303 18:53:57.3 13:03:44.0 B1855+09 18:57:36.3 09:43:17.2 J1910+1256 19:10:09.7 12:56:25.5 J2017+0603 20:17:22.7 06:03:05.6 J2214+3000 22:14:38.8 30:00:38.2 J2317+1439 23:17:09.2 14:39:31.2 J0023+0923 00:23:16.9 9:23:23.8 3


J0030+0451 00:30:27.4 04:51:39.7 Session B: J1738+0333 17:38:53.9 03:33:10.8 J1903+0327 19:03:07.3 03:27:42.0 J1944+0907 19:44:09.3 09:07:23.2 B1953+29 19:55:27.8 29:08:43.5 J2043+1711 20:43:20.9 17:11:28.9 Session C: J1741+1351 17:41:31.2 13:51:44.2 J1923+2515 19:23:22.5 25:15:40.6 B1937+21 19:39:38.5 21:34:59.1 J1949+3106 19:49:29.6 31:06:03.8

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