Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/vscience/schedule/2015Spring/StovalltagP2825.pdf Дата изменения: Tue Sep 9 17:24:54 2014 Дата индексирования: Mon Apr 11 17:07:21 2016 Кодировка: Поисковые слова: рер р р р р р р р р р р р р р

Proposal Identification No.:

P2825 Arecibo Observatory

Date Received: 2014-Sep-02 12:54:21 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2014. This proposal has been submitted before. The previous proposal number is P2825. 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: Regular Pulsars Galactic 54 27 124.5 0.5 100-500 GB

Followup Timing of Sources Discovered in the Arecibo Observatory 327 MHz

Drift Survey
ABSTRACT: The Arecibo Observatory 327 MHz Drift Scan survey has discovered 46 new radio pulsars. We recently added a new algorithm to automatically identify single pulses that are likely to be of astrophysical origin. This new algorithm has resulted in the discovery of 12 new sources, comprised of pulsars with variable emission and rotating radio transients (RRATs). Some of these sources are being followed up using time from previous successful observing proposals. We are requesting 81 hours to follow-up 10 new sources, including a new mode switching pulsar and 5 new RRATs. These observations will allow us to very precisely measure the sources' spin and astrometric parameters as well as to allow us to study the variability of these new sources. Outreach Abstract: The Arecibo Observatory 327 MHz Drift survey utilizes time in which the telescope is not fully functional such as during times in which the telescope is undergoing repair as well as time which is under-requested to search the sky for a type of star called a radio pulsar. Radio pulsars are very dense ob jects called neutron stars that emit beams of radio waves out of their magnetic poles. As the star spins, the beams of radio waves sweep over the Arecibo Observatory causing a very regular pulse appearing as if it is a pulsating star (pulsar). This survey has detected 46 new pulsars total and 14 within the past year. We are taking data to monitor ten of these newly discovered sources.

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Name Kevin Stovall Julia Deneva

Institution University of New Mexico Naval Research Laboratory

E-mail stovall.kevin@gmail.com julia.deneva@gmail.com

Phone 3252262495

Student no no

Additional Authors
Paulo Freire (pfreire@mpifr-bonn.mpg.de), J. Martinez (joey.martinez10@gmail.com), S. Bates (sam.d.bates@gmail.com), F. Jenet (fredricka jenet@gmail.com), M. A. McLaughlin (maura.mclaughlin@mail.wvu.edu), M. Bagchi (manjari.bagchi@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 ­ ­ ­ ­

Days Needed at This Interval

Time Constraints (Must Be Justified in the Prop osal Text) Ё Details for these observations are described in the Proposed Observations" section of the proposal, including 5 LST ranges. For each LST range, we request a set of observations to get initial phase connection spaced on days 1,2,3,5,10, and 20. We then request an observation be scheduled on day 30 2


(plus or minus 3 days), which begins our monthly monitoring of these sources in which we request observations be scheduled every 30 days (plus or minus 3 days) for the remainder of the semester. The total number of days for this semester for each LST range is 12.

Next Semester Time Request

Begin ­ End Interval­Interval ­ ­ ­ ­

Days Needed at This Interval

Time Constraints (Must Be Justified in the Prop osal Text) We request continued monitoring every 30 days (plus or minus 30 days). The total number of days for this semester for each LST range is 6.

Section I I I - Instruments Needed
430 G L-wide 327

Atmospheric Observation Instruments:

Sp ecial Equipment or setup: The 327 MHz receiver is our primary receiver. We will occasionally use the 430 MHz and L-wide receiver to investigate the spectral properties of our sources, but only after we know their positions very well.

Section IV - RFI Considerations Frequency Ranges Planned

This proposal requires Iridium RFI protection at 1612 MHz between 10pm and 6am EST. 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
Target list with position and LST rise-set are included in Table 1 of the scientific justification.

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