Pulsar-timing analyses are sensitive to errors in the solar-system
ephemerides (SSEs) that timing models utilise to estimate the location of the
solar-system barycentre, the quasi-inertial reference frame to which all
recorded pulse times-of-arrival are referred. Any error in the SSE will affect
all pulsars, therefore pulsar timing arrays (PTAs) are a suitable tool to
search for such errors and impose independent constraints on relevant physical
parameters. We employ the first data release of the International Pulsar Timing
Array to constrain the masses of the planet-moons systems and to search for
possible unmodelled objects (UMOs) in the solar system. We employ ten SSEs from
two independent research groups, derive and compare mass constraints of
planetary systems, and derive the first PTA mass constraints on asteroid-belt
objects. Constraints on planetary-system masses have been improved by factors
of up to 20 from the previous relevant study using the same assumptions, with
the mass of the Jovian system measured at 9.5479189(3)$\times10^-4$
$M_ødot$. The mass of the dwarf planet Ceres is measured at
4.7(4)$\times10^-10$ $M_ødot$. We also present the first sensitivity
curves using real data that place generic limits on the masses of UMOs, which
can also be used as upper limits on the mass of putative exotic objects. For
example, upper limits on dark-matter clumps are comparable to published limits
using independent methods. While the constraints on planetary masses derived
with all employed SSEs are consistent, we note and discuss differences in the
associated timing residuals and UMO sensitivity curves.
Description
Studying the solar system with the International Pulsar Timing Array
%0 Generic
%1 caballero2018studying
%A Caballero, R. N.
%A Guo, Y. J.
%A Lee, K. J.
%A Lazarus, P.
%A Champion, D. J.
%A Desvignes, G.
%A Kramer, M.
%A Plant, K.
%A Arzoumanian, Z.
%A Bailes, M.
%A Bassa, C. G.
%A Bhat, N. D. R.
%A Brazier, A.
%A Burgay, M.
%A Burke-Spolaor, S.
%A Chamberlin, S. J.
%A Chatterjee, S.
%A Cognard, I.
%A Cordes, J. M.
%A Dai, S.
%A Demorest, P.
%A Dolch, T.
%A Ferdman, R. D.
%A Fonseca, E.
%A Gair, J. R.
%A Garver-Daniels, N.
%A Gentile, P.
%A Gonzalez, M. E.
%A Graikou, E.
%A Guillemot, L.
%A Hobbs, G.
%A Janssen, G. H.
%A Karuppusamy, R.
%A Keith, M. J.
%A Kerr, M.
%A Lam, M. T.
%A Lasky, P. D.
%A Lazio, T. J. W.
%A Levin, L.
%A Liu, K.
%A Lommen, A. N.
%A Lorimer, D. R.
%A Lynch, R. S.
%A Madison, D. R.
%A Manchester, R. N.
%A McKee, J. W.
%A McLaughlin, M. A.
%A McWilliams, S. T.
%A Mingarelli, C. M. F.
%A Nice, D. J.
%A Osłowski, S.
%A Palliyaguru, N. T.
%A Pennucci, T. T.
%A Perera, B. B. P.
%A Perrodin, D.
%A Possenti, A.
%A Ransom, S. M.
%A Reardon, D. J.
%A Sanidas, S. A.
%A Sesana, A.
%A Shaifullah, G.
%A Shannon, R. M.
%A Siemens, X.
%A Simon, J.
%A Spiewak, R.
%A Stairs, I.
%A Stappers, B.
%A Stinebring, D. R.
%A Stovall, K.
%A Swiggum, J. K.
%A Taylor, S. R.
%A Theureau, G.
%A Tiburzi, C.
%A Toomey, L.
%A van Haasteren, R.
%A van Straten, W.
%A Verbiest, J. P. W.
%A Wang, J. B.
%A Zhu, X. J.
%A Zhu, W. W.
%D 2018
%K ephemerides mass solar_system
%R 10.1093/mnras/sty2632
%T Studying the solar system with the International Pulsar Timing Array
%U http://arxiv.org/abs/1809.10744
%X Pulsar-timing analyses are sensitive to errors in the solar-system
ephemerides (SSEs) that timing models utilise to estimate the location of the
solar-system barycentre, the quasi-inertial reference frame to which all
recorded pulse times-of-arrival are referred. Any error in the SSE will affect
all pulsars, therefore pulsar timing arrays (PTAs) are a suitable tool to
search for such errors and impose independent constraints on relevant physical
parameters. We employ the first data release of the International Pulsar Timing
Array to constrain the masses of the planet-moons systems and to search for
possible unmodelled objects (UMOs) in the solar system. We employ ten SSEs from
two independent research groups, derive and compare mass constraints of
planetary systems, and derive the first PTA mass constraints on asteroid-belt
objects. Constraints on planetary-system masses have been improved by factors
of up to 20 from the previous relevant study using the same assumptions, with
the mass of the Jovian system measured at 9.5479189(3)$\times10^-4$
$M_ødot$. The mass of the dwarf planet Ceres is measured at
4.7(4)$\times10^-10$ $M_ødot$. We also present the first sensitivity
curves using real data that place generic limits on the masses of UMOs, which
can also be used as upper limits on the mass of putative exotic objects. For
example, upper limits on dark-matter clumps are comparable to published limits
using independent methods. While the constraints on planetary masses derived
with all employed SSEs are consistent, we note and discuss differences in the
associated timing residuals and UMO sensitivity curves.
@misc{caballero2018studying,
abstract = {Pulsar-timing analyses are sensitive to errors in the solar-system
ephemerides (SSEs) that timing models utilise to estimate the location of the
solar-system barycentre, the quasi-inertial reference frame to which all
recorded pulse times-of-arrival are referred. Any error in the SSE will affect
all pulsars, therefore pulsar timing arrays (PTAs) are a suitable tool to
search for such errors and impose independent constraints on relevant physical
parameters. We employ the first data release of the International Pulsar Timing
Array to constrain the masses of the planet-moons systems and to search for
possible unmodelled objects (UMOs) in the solar system. We employ ten SSEs from
two independent research groups, derive and compare mass constraints of
planetary systems, and derive the first PTA mass constraints on asteroid-belt
objects. Constraints on planetary-system masses have been improved by factors
of up to 20 from the previous relevant study using the same assumptions, with
the mass of the Jovian system measured at 9.5479189(3)$\times10^{-4}$
$M_{\odot}$. The mass of the dwarf planet Ceres is measured at
4.7(4)$\times10^{-10}$ $M_{\odot}$. We also present the first sensitivity
curves using real data that place generic limits on the masses of UMOs, which
can also be used as upper limits on the mass of putative exotic objects. For
example, upper limits on dark-matter clumps are comparable to published limits
using independent methods. While the constraints on planetary masses derived
with all employed SSEs are consistent, we note and discuss differences in the
associated timing residuals and UMO sensitivity curves.},
added-at = {2018-10-25T13:06:19.000+0200},
author = {Caballero, R. N. and Guo, Y. J. and Lee, K. J. and Lazarus, P. and Champion, D. J. and Desvignes, G. and Kramer, M. and Plant, K. and Arzoumanian, Z. and Bailes, M. and Bassa, C. G. and Bhat, N. D. R. and Brazier, A. and Burgay, M. and Burke-Spolaor, S. and Chamberlin, S. J. and Chatterjee, S. and Cognard, I. and Cordes, J. M. and Dai, S. and Demorest, P. and Dolch, T. and Ferdman, R. D. and Fonseca, E. and Gair, J. R. and Garver-Daniels, N. and Gentile, P. and Gonzalez, M. E. and Graikou, E. and Guillemot, L. and Hobbs, G. and Janssen, G. H. and Karuppusamy, R. and Keith, M. J. and Kerr, M. and Lam, M. T. and Lasky, P. D. and Lazio, T. J. W. and Levin, L. and Liu, K. and Lommen, A. N. and Lorimer, D. R. and Lynch, R. S. and Madison, D. R. and Manchester, R. N. and McKee, J. W. and McLaughlin, M. A. and McWilliams, S. T. and Mingarelli, C. M. F. and Nice, D. J. and Osłowski, S. and Palliyaguru, N. T. and Pennucci, T. T. and Perera, B. B. P. and Perrodin, D. and Possenti, A. and Ransom, S. M. and Reardon, D. J. and Sanidas, S. A. and Sesana, A. and Shaifullah, G. and Shannon, R. M. and Siemens, X. and Simon, J. and Spiewak, R. and Stairs, I. and Stappers, B. and Stinebring, D. R. and Stovall, K. and Swiggum, J. K. and Taylor, S. R. and Theureau, G. and Tiburzi, C. and Toomey, L. and van Haasteren, R. and van Straten, W. and Verbiest, J. P. W. and Wang, J. B. and Zhu, X. J. and Zhu, W. W.},
biburl = {https://www.bibsonomy.org/bibtex/2ac8a561b862cdd26ebac815187d38cd6/mkretlow},
description = {Studying the solar system with the International Pulsar Timing Array},
doi = {10.1093/mnras/sty2632},
interhash = {fd8f686bc57cb1287b738ff41e5811b0},
intrahash = {ac8a561b862cdd26ebac815187d38cd6},
keywords = {ephemerides mass solar_system},
note = {cite arxiv:1809.10744Comment: Accepted for publication by the Monthly Notices of the Royal Astronomical Society},
timestamp = {2018-10-25T13:06:19.000+0200},
title = {Studying the solar system with the International Pulsar Timing Array},
url = {http://arxiv.org/abs/1809.10744},
year = 2018
}