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Proposal Identification No.:

P2989 Arecibo Observatory

Date Received: 2015-Mar-02 15:44:30 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Mar 1 2015. 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 27

1.5 hours 100-500 GB

Expanding the NANOGrav Pulsar Timing Array

Direct detection of gravitational waves (GWs) is a ma jor goal in experimental physics and will open an entirely new astronomical spectrum. Precision millisecond pulsar (MSP) 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, so NANOGrav is aggressively searching for pulsars suitable for inclusion in PTAs. In this proposal, we request time to observe eight newly-discovered pulsars, and three older pulsar discoveries that have not yet been evaluated using new instrumentation. We expect several of these pulsars may 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 Elizabeth C Ferrara Paul B Demorest

Institution University of Maryland, College Park NRAO

E-mail Elizabeth.C.Ferrara@nasa.gov pdemores@nrao.edu

Phone 301-286-7057 575-835-7248

Student no no

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Additional Authors
David J. Nice, niced@lafayette.edu Ingrid Stairs, stairs@astro.ubc.ca Scott Ransom, sransom@nrao.edu Zaven Arzoumanian, zaven.arzoumanian@nasa.gov Glenn Jones, glenn.caltech@gmail.com Michael T. Lam (grad), Michael Lam mtl82@cornell.edu Paul S. Ray, paul.ray@nrl.navy.mil Kevin Stovall, kstovall@unm.edu Joseph Swiggum (grad), swiggumj@gmail.com Weiwei Zhu, zhuww@phas.ubc.ca Robert Ferdman, rferdman@physics.mcgill.ca Maura McLaughlin, maura.mclaughlin@mail.wvu.edu NANOGrav Collaboration, nano-time@nanograv.org Emmanuel Fonseca (grad), efonseca@phas.ubc.ca Timothy Pennucci (grad), ttp4tx@virginia.edu

Jim Cordes, cordes@astro.cornell.edu Ryan S. Lynch, rlynch@nrao.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 04:30 ­ 08:00 11:00 ­ 14:20 12:00 ­ 13:00 16:00 ­ 21:30

Days Needed at This Interval 2 2 2 2

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

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J0557+1551, J0621+2514 and J0709+0458 can be observed together in a 3.5-hour session, beginning near 4.5h LST. J1142+0119, B1257+12, and J1312+0051 can be observed together in a 3-hour session, beginning near 11h LST. J1630+3734, J1745+1017, J1905+0400, J1935+1726, and J2042+0246 can be observed together in a 5.5-hour session, beginning near 16h LST. J1239+3232 will be observed in individual 1-hour sessions. The two sessions for each source should be spaced apart by at least two weeks. 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: All observations will use the PUPPI pulsar backend.

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
J0557+1551 05:57:31.4 15:50:06.0 04:36:38 07:20:11 J0621+2514 06:21:10.9 25:14:03.0 05:02:31 07:41:45 J0709+0458 07:09:08.4 04:58:51.5 06:10:53 08:09:02 J1142+0119 11:42:50.1 01:19:35.5 11:03:57 12:23:19 J1239+3239 12:39:26.5 32:39:22.4 11:39:33 13:40:51 B1257+12 13:00:03.6 12:40:56.5 11:42:37 14:19:04 J1312+0051 13:12:46.6 00:51:00.1 12:37:30 13:49:39 J1630+3734 16:30:36.5 37:34:42.1 16:11:00 16:51:18 J1745+1017 17:45:33.8 10:17:52.5 16:32:01 19:00:32 J1905+0400 19:05:28.3 04:00:10.9 18:10:59 20:01:28 3


J1935+1726 19:35:03.9 17:26:28.5 18:13:00 20:58:28 J2042+0246 20:42:11.0 02:46:14.4 19:53:30 21:32:22

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