A dataset provided by the European Space Agency

Name: PSR J1734-3333: A Magnetar ProgenitorquestionMark
Published: 2014-04-12T00:00:00Z

Proposal ID	069296
Title	PSR J1734-3333: A Magnetar Progenitor?
Download Data Associated to the proposal	https://nxsa.esac.esa.int/nxsa-sl/servlet/data-action-aio?obsno=0692960101
DOI	https://doi.org/10.5270/esa-aevwlb7
Principal Investigator, PI	Prof Victoria Kaspi
Abstract	We propose X-ray observations of the radio pulsar PSR J1734-3333, a possiblemagnetar progenitor. This source, a 1.2 s radio pulsar, has inferred surfacemagnetic field 5.2e13 G, well above the quantum critical field and very close tothose of bona fide magnetars. In radio timing observations we have recentlymeasured a stable braking index for this source, n=0.9+/-0.2. So low a brakingindex is unprecedented and suggests effective magnetic field growth, such thatthis source may soon become some form of magnetar. A previous deep XMMobservation was significantly contaminated by background flaring. Here werequest an observation to replace the exposure time lost due to flares, in orderto constrain the sources spectral properties and search for pulsations.
Publications	The Million Optical - Radio/X-ray Associations (MORX) Catalogue \|Flesch, Eric W., \| PASA \| 33-52 \| 2016 \| 2016PASA...33...52F \| http://ui.adsabs.harvard.edu/#abs/2016PASA...33...52F Classification of 4XMM-DR9 sources by machine learning \|Zhang, Yanxia, Zhao, Yongheng, \| MNRAS \| 503-5263 \| 2021 \| 2021MNRAS.503.5263Z \| http://ui.adsabs.harvard.edu/#abs/2021MNRAS.503.5263Z From Active Stars to Black Holes: A Discovery Tool for Galactic X-Ray Sources \|Rodriguez, Antonio C., \| PASP \| 136-054201 \| 2024 \| 2024PASP..136e4201R \| http://ui.adsabs.harvard.edu/#abs/2024PASP..136e4201R Robust constraints on feebly interacting particles using XMM-Newton \|Luque, Pedro De la Torre, Balaji, Shyam, \| PhRvD \| 109-L101305 \| 2024 \| 2024PhRvD.109j1305L \| http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j1305L Multimessenger search for electrophilic feebly interacting particles from supernovae \|Luque, Pedro De la Torre, Balaji, Shyam, \| PhRvD \| 109-103028 \| 2024 \| 2024PhRvD.109j3028L \| http://ui.adsabs.harvard.edu/#abs/2024PhRvD.109j3028L Importance of Cosmic-Ray Propagation on Sub-GeV Dark Matter Constraints \|De la Torre Luque, Pedro, Balaji, Shyam, \| ApJ \| 968-46 \| 2024 \| 2024ApJ...968...46D \| http://ui.adsabs.harvard.edu/#abs/2024ApJ...968...46D
Instrument	EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage	2013-03-24T07:32:56Z/2013-03-25T01:18:12Z
Version	17.56_20190403_1200
Mission Description	The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earths atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
Creator Contact	https://www.cosmos.esa.int/web/xmm-newton/xmm-newton-helpdesk
Date Published	2014-04-12T00:00:00Z
Keywords	"XMM", "magnetar progenitor ?.", "magnetar progenitor", "radio pulsar", "sources spectral properties", "bona fide magnetar", "braking index", "deep xmm", "stable braking index", "background flaring", "psr j1734 3333", "exposure time lost"
Publisher And Registrant	European Space Agency
Credit Guidelines	European Space Agency, Prof Victoria Kaspi, 2014, 'PSR J1734-3333: A Magnetar ProgenitorquestionMark', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-aevwlb7