2009A&A...497..451M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST21:19:10

2009A&A...497..451M - Astronomy and Astrophysics, volume 497, 451-455 (2009/4-2)

VLT/NACO near-infrared observations of the transient radio magnetar 1E 1547.0-5408.

MIGNANI R.P., REA N., TESTA V., ISRAEL G.L., MARCONI G., MEREGHETTI S., JONKER P., TUROLLA R., PERNA R., ZANE S., LO CURTO G. and CHATY S.

Abstract (from CDS):

Despite about a decade of observations, very little is known about the optical and infrared (IR) emission properties of the soft gamma-ray repeaters (SGRs) and of the anomalous X-ray pulsars (AXPs), the magnetar candidates, and about the physical processes which drive their emission at these wavelengths. This is mainly due to the limited number of identifications achieved so far, five in total, and to the sparse spectral coverage obtained from multi-band optical/IR photometry. The aim of this work is to search for a likely candidate counterpart to the recently discovered transient radio AXP 1E 1547.0-5408.We performed the first deep near-IR (NIR) observations (Ks band) of 1E 1547.0-5408 with the Very Large Telescope (VLT) on three nights (July 8th, 12th, and August 17th), after the X-ray source rebrightening and during the subsequent decay reported around June 2007.We detected four objects within, or close to, the 3σ radio position of 1E 1547.0-5408. The faintest of them (object 1) has a brightness Ks=20.27 ±0.05, which would yield an unabsorbed X-ray-to-NIR flux ratio FX/FKs∼800 for 1E 1547.0-5408, i.e. on average lower than those derived for other magnetars. The non-detection of object 1 on the nights of July 8th and August 17th only allowed us to set an upper limit of ΔKs∼0.2 on its NIR variability, which prevented us from searching for correlations with the radio or X-ray flux. We detected no other object at the radio position down to a limit of Ks ∼21.7 (at 5 σ), computed in our deepest VLT image (July 12th). From our observations we cannot confidently propose a NIR counterpart to 1E 1547.0-5408. More NIR observations of object 1, e.g. to determine its colors and to monitor variability, would be conclusive to determine whether or not it can be considered a plausible candidate.

Abstract Copyright:

Journal keyword(s): stars: neutron - stars: pulsars: individual: 1E 1547.0-5408 - infrared: general

Nomenclature: Fig. 1, Table 2: [MRT2009] N (Nos 1-4).

Simbad objects: 12

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Number of rows : 12

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 J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 505 0
2 GRB 080822 gB 05 01 05.0 +45 16 20           ~ 70 0
3 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 512 1
4 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 378 0
5 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 331 1
6 SNR G327.2-00.1 SNR 15 50 55 -54 18.0           ~ 60 1
7 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 261 0
8 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1097 2
9 AX J1809.8-1943 Psr 18 09 51.07 -19 43 51.8           ~ 364 0
10 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 233 1
11 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 779 0
12 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 585 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-21:19:10

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