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Дата изменения: Tue Sep 9 17:24:58 2014
Дата индексирования: Mon Apr 11 17:06:47 2016
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Proposal Identification No.:

P2945 Arecibo Observatory

Date Received: 2014-Sep-02 16:30:01 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2014. 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: The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) is a collaboration of scientists and students that uses many radio pulsars as a type of Galactic-scale detector in an effort to be the first to directly detect gravitational waves (GWs). The current NANOGrav observing program is optimized for the detection of a stochastic background of GWs from unresolved sources in the Universe, but not robust for the detection of resolvable, individual GW sources. In this proposal, we request an increased observing cadence for five of the best-timed NANOGrav pulsars in an effort to boost our sensitivity to individual GW sources as shown in recent studies and simulations described in the accompanying text. These measurements will be crucial for understanding largely unconstrained astrophysical processes influencing the population of potential GW sources, such as merging supermassive black-hole binary systems. Outreach Abstract: Los pulsares han demostrado ser laboratorios excepcionales para la comprension de la fisica gravitacional en ambientes extremos. Estamos proponiendo a observar cinco pulsars que son parte del grupo "North American Nanohertz Observatory for Gravitational Waves" (NANOGrav), que es una colaboracion de cientificos y estudiantes tratando de ver directamente las ondas gravitacionales. NANOGrav ahora sirve para detectar las ondas gravitacionales de todos sistemas orbitales de los agujeros negros en el Universo, pero no sirve bien para detectar y entender las ondas gravitacionales de sistemas individuales. Ahora estamos tratando de mejorar las observaciones de NANOGrav para detectar estas ondas gravitacionales de uniqos sistemas y entender la fisica de los agujeros negros. Large Pulsars Galactic 130 130 0 30 minutes over 500 GB

An Improved Single-Source Detector for the North American Nanohertz Observatory for Gravitational Waves

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Name Emmanuel Fonseca Ingrid H Stairs

Institution The University of British Columbia The University of British Columbia

E-mail efonseca@phas.ubc.ca stairs@astro.ubc.ca

Phone 604-218-5426 604-822-6796

Student G no

Additional Authors
Xavier Siemens siemens@gravity.phys.uwm.edu Jim Cordes cordes@astro.cornell.edu Shamibrata Chatterjee shami@astro.cornell.edu Justin Ellis justin.ellis18@gmail.com Dustin Madison (graduate) drm252@cornell.edu Paul Demorest - pdemores@nrao.edu David Nice - niced@lafayette.edu Scott Ransom - sransom@nrao.edu Zaven Arzoumanian zaven.arzoumanian@nasa.gov Tim Dolch - td288@cornell.edu Robert Ferdman rferdman@physics.mcgill.ca Glenn Jones glenn.caltech@gmail.com Maura McLaughlin maura.mclaughlin@mail.wvu.edu Timothy Pennucci (graduate) ttp4tx@virginia.edu Kevin Stovall stovall.kevin@gmail.com Joseph Swiggum (graduate) swiggumj@gmail.com Weiwei Zhu - zhuww@phas.ubc.ca NANOGrav Collaboration nano-time@nanograv.org

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 00:00 01:00 15:30 16:30 16:30 17:30 20:00 21:00

Days Needed at This Interval 26 26 26 26

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Time Constraints (Must Be Justified in the Prop osal Text) As we discuss in our attached proposal, we prefer to observe five radio pulsars, each for one hour per observing epoch, for 26 epochs during each semester for each source or 52 epochs for the whole observing year (52 x 5 = 260 hours total for all five sources). There were only four entries allowed in the proposal cover sheet, though all five pulsars and their LST ranges are listed in the "List of Targets" below. However, we are very flexible about when and how these sessions are scheduled during the semester/year, as these pulsars need not be observed within the same day or at equally spaced epochs. Moreover, we can be scheduled for "filler" time and observe any of these pulsars in sessions as short as 30-minutes using a single receiver. The key point is that any additional data on these five pulsars, beyond the standard NANOGrav observing program, will increase our sensitivity to localized GW sources. Our ideal program, with 52 observing epochs per pulsar per year, would double our sensitivity to such GW sources as described in the attached proposal justification.

Next Semester Time Request

Begin End IntervalInterval 00:00 01:00 15:30 16:30 16:30 17:30 20:00 21:00

Days Needed at This Interval 26 26 26 26

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

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

Atmospheric Observation Instruments:

Sp ecial Equipment or setup: We will also continue to use the PUPPI data acquisition system currently operating at Arecibo Observatory for high-precision, real-time measurements of TOAs from each pulsar.

Section IV - RFI Considerations Frequency Ranges Planned
420-440 1150-1800 1700-2400 3

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
PSR PSR PSR PSR PSR J0030+0451 J1640+2224 J1713+0747 J2043+1711 J2317+1439 00h30m, 16h40m, 17h13m, 20h43m, 23h17m, 04d51m, 22d24m, 07d47m, 17d11m, 14d39m, 23:31-01:29 15:18-18:03 16:05-18:22 19:21-22:06 21:56-00:38

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