2011A&A...533A.101M


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST11:59:32

2011A&A...533A.101M - Astronomy and Astrophysics, volume 533A, 101-101 (2011/9-1)

VLT observations of the two Fermi pulsars PSR J1357-6429 and PSR J1048-5832.

MIGNANI R.P., SHEARER A., DE LUCA A., MORAN P., COLLINS S. and MARELLI M.

Abstract (from CDS):

Optical observations of pulsars are crucial to studying the neutron star properties from the structure and composition of the interior to the properties and geometry of the magnetosphere. Historically, X and γ-ray observations have paved the way to pulsar optical identifications. The launch of the Fermi Gamma-ray Space Telescope opened new perspectives in the optical-to-γ-ray studies of neutron stars with the detection of more than 80 γ-ray pulsars. Here, we aim to search for optical emission from two Fermi pulsars that are interesting targets on the basis of their spin-down age, energetics, and distance. PSR J1357-6429 is a Vela-like pulsar (P=166.1ms; τ=7.31kyr), at a distance of ∼2.4kpc with a rotational energy loss rate {dot}(E)∼3x1036erg/s. PSR J1048-5832 is also a Vela-like (P=123.6ms; τ=20.3kyr) pulsar at a distance of ∼2.7kpc and with a {dot}(E)∼2x1036erg/s. The two pulsars and their pulsar wind nebulae (PWNe) are also detected in X-rays by Chandra and XMM-Newton. No deep optical observations of these two pulsars have been reported so far. We used multi-band optical images (V,R,I) taken with the Very Large Telescope (VLT) and available in the European Southern Observatory (ESO) archive to search for, or put tight constraints on, their optical emission. We re-assessed the positions of the two pulsars from the analyses of all the available Chandra observations and the comparison with the published radio coordinates. For PSR J1357-6429, this yielded a tentative proper motion µ= 0.17±0.055"/yr (70°±15° position angle). We did not detect any candidate counterparts to PSR J1357-6429 and PSR J1048-5832 down to V∼27 and ∼27.6, respectively, although for the former we found possible evidence of a faint, unresolved object at the Chandra position. Our limits imply an efficiency in converting spin-down power into optical luminosity ≲7x10–7 and ≲6x10–6, possibly close to that of the Vela pulsar. Observations with the Hubble Space Telescope (HST) are required to identify PSR J1357-6429 against nearby field stars. Owing to the high extinction (AV∼5) and the presence of a molecular cloud complex, near-infrared observations of PSR J1048-5832 are better suited to spotting its candidate counterpart.

Abstract Copyright:

Journal keyword(s): stars: neutron - pulsars: individual: PSR J1357-6429 - pulsars: individual: PSR J1048-5832

CDS comments: Paragraph 2.1 3EG J1048-5048 is s a misprint for 3EG J1048-5840.

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 PSR J0108-1431 Psr 01 08 08.29 -14 31 48.5           ~ 92 0
2 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4831 1
3 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5652 4
4 PSR B0613-02.0 Psr 06 13 43.9759 -02 00 47.228           ~ 203 1
5 NAME Geminga Psr 06 33 54.153 +17 46 12.91           ~ 1096 0
6 PSR B0656+14 Psr 06 59 48.183 +14 14 21.54   24.85 24.90     ~ 764 1
7 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2074 1
8 PSR B0950+08 Psr 09 53 09.3 +07 55 36           ~ 699 2
9 PSR B1046-58 Psr 10 48 12.391 -58 32 02.68           ~ 230 0
10 PSR B1055-52 Psr 10 57 58.970 -52 26 56.52           ~ 682 0
11 PSR J1357-6429 Psr 13 57 02.525 -64 29 29.89           ~ 120 1
12 PSR B1509-58 Psr 15 13 55.52 -59 08 08.8           ~ 799 1
13 PSR B1706-44 Psr 17 09 42.62 -44 29 05.8           ~ 579 1
14 PSR B1929+10 Psr 19 32 13.79 +10 59 33.2           ~ 698 0
15 PSR B2223+65 Psr 22 25 52.36 +65 35 33.8           ~ 290 0

    Equat.    Gal    SGal    Ecl

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2020.10.24-11:59:32

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