E-resources
Open access
-
Arzoumanian, Zaven; Brazier, Adam; Burke-Spolaor, Sarah; Chamberlin, Sydney; Chatterjee, Shami; Christy, Brian; Cordes, James M; Cornish, Neil J; Crawford, Fronefield; Cromartie, H Thankful; Crowter, Kathryn; DeCesar, Megan E; Demorest, Paul B; Dolch, Timothy; Ellis, Justin A; Ferdman, Robert D; Ferrara, Elizabeth C; Fonseca, Emmanuel; Garver-Daniels, Nathan; Gentile, Peter A; Halmrast, Daniel; Huerta, Eliu; Jenet, Fredrick A; Jessup, Cody; Jones, Glenn; Jones, Megan L; Kaplan, David L; Lam, Michael T; Lazio, T Joseph W; Levin, Lina; Lommen, Andrea; Lorimer, Duncan R; Luo, Jing; Lynch, Ryan S; Madison, Dustin; Matthews, Allison M; McLaughlin, Maura A; McWilliams, Sean T; Mingarelli, Chiara; Ng, Cherry; Nice, David J; Pennucci, Timothy T; Ransom, Scott M; Ray, Paul S; Siemens, Xavier; Simon, Joseph; Spiewak, Renee; Stairs, Ingrid H; Stinebring, Daniel R; Stovall, Kevin; Swiggum, Joseph K; Taylor, Stephen R; Vallisneri, Michele; Rutger van Haasteren; Vigeland, Sarah J; Zhu, Weiwei
arXiv.org, 04/2018Paper, Journal Article
We present high-precision timing data over time spans of up to 11 years for 45 millisecond pulsars observed as part of the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) project, aimed at detecting and characterizing low-frequency gravitational waves. The pulsars were observed with the Arecibo Observatory and/or the Green Bank Telescope at frequencies ranging from 327 MHz to 2.3 GHz. Most pulsars were observed with approximately monthly cadence, with six high--timing-precision pulsars observed weekly, and all were observed at widely separated frequencies at each observing epoch in order to fit for time-variable dispersion delays. We describe our methods for data processing, time-of-arrival (TOA) calculation, and the implementation of a new, automated method for removing outlier TOAs. We fit a timing model for each pulsar that includes spin, astrometric, and, if necessary, binary parameters, in addition to time-variable dispersion delays and parameters that quantify pulse-profile evolution with frequency. The new timing solutions provide three new parallax measurements, two new Shapiro delay measurements, and two new measurements of large orbital-period variations. We fit models that characterize sources of noise for each pulsar. We find that 11 pulsars show significant red noise, with generally smaller spectral indices than typically measured for non-recycled pulsars, possibly suggesting a different origin. Future papers will use these data to constrain or detect the signatures of gravitational-wave signals.
Author
![loading ... loading ...](themes/default/img/ajax-loading.gif)
Shelf entry
Permalink
- URL:
Impact factor
Access to the JCR database is permitted only to users from Slovenia. Your current IP address is not on the list of IP addresses with access permission, and authentication with the relevant AAI accout is required.
Year | Impact factor | Edition | Category | Classification | ||||
---|---|---|---|---|---|---|---|---|
JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
Select the library membership card:
If the library membership card is not in the list,
add a new one.
DRS, in which the journal is indexed
Database name | Field | Year |
---|
Links to authors' personal bibliographies | Links to information on researchers in the SICRIS system |
---|
Source: Personal bibliographies
and: SICRIS
The material is available in full text. If you wish to order the material anyway, click the Continue button.