Re-submission with duplicate of failed visit 06
449642730
----- Attempting Submission 1 (Fri Jan 31 09:44:29 GMT 2025) -----
HST Phase II Proposal 17927 successfully submitted.
Receipt: # 17927-1
----- Attempting Submission 2 (Wed Apr 23 09:11:24 GMT 2025) -----
Unveiling the origin of magnetars through a large proper motion sample
We propose WFC3/IR imaging in F125W and F160W of 15 Galactic magnetars, closely matching observations taken in 2018 and 2020 in order to precisely measure the proper motions of their faint NIR counterparts. The origin of magnetars remains unclear. By re-measuring their positions with milliarcsecond precision ~6 years later, with the same instrument and using the 2018-2020 imaging as a reference, we will increase the number of magnetars with a precise transverse velocity measurement - or a strong upper limits on the velocity - by up to a factor of two. Combined with estimates for the magnetar ages, we can trace them back to an inferred birth site, to search for supernova remnants or star forming regions (or a lack thereof). Our proposed program will move us out of the realm of small number statistics, allowing a statistically robust comparison with the peculiar velocity distrbution of other neutron stars (namely pulsars). This programme will therefore reveal much about the nature and origin of magnetars. This cycle 32 call for bridge programs is the last chance to obtain HST proper motions for these systems; it also acts as pathfinder programme for broader JWST studies in future cycles which could target proper motion measurements of a wider array of Galactic systems.
Imaging strategy and S/N: WFC3/IR observations of 15 magnetars in both F125W and F160W. These were previously imaged with HST between 2018-2020. Each field has 2400s (1 orbit) of exposure time, split between the two filters, with the exposures in each filter split with the WFC3-IR-DITHER-LINE-3PT dither pattern. The faintest counterpart candidate in the sample has magnitude F160W(AB)~25. Our exposure time yields a S/N of 20 for point sources of this magnitude, and gives 3 sigma limiting magnitudes of ~26.8. This ensures re-detections of the counterparts in both bands, even if they are variable by 1-2 mag (typical for magnetars) and fainter in this epoch. Total time: 15 targets will be observed for 1 orbit each, with half an orbit per filter (F125W+F160W), each split into three 400s dithered exposures. The total time usage is therefore 15 orbits.
The team has extensive experience with HST, compact object research, and the application of HST in other areas, particularly transient astronomy. We have previously had HST programmes approved to observe Galactic magnetar counterparts in the NIR, and have obtained several hundred orbits of HST time dedicated to the study of gamma-ray bursts, extreme supernovae, tidal disruptions and their host galaxies.
We have experience from design to reduction to publication. Recent publications on magnetars include Chrimes et al. (2021), Chrimes et al. (2022a,b) and Lyman et al. (2022, using HST data to measure the proper motion of SGR1935+2154). Other highlights include some of the seminal studies of magnetars (e.g. Kouveliotou et al. 1999), GRB host galaxies with HST (e.g. Fruchter et al. 2006), the identification of GRBs and their host galaxies at the highest redshift (e.g. Tanvir et al. 2009, Tanvir et al. 2012), the location and host galaxy studies for tidal disruption events (e.g. Levan et al. 2011), and the first Hubble Space Telescope observations of the EM counterpart of a gravitational wave source (Levan et al. 2017, Tanvir et al. 2017, Lyman et al. 2018). The PI has extensive experience with the analysis of HST observations (e.g Chrimes et al. 2019, Chrimes et al. 2022a, Chrimes et al. 2024a,b), and is currently an independent research fellow. We therefore have the experience and the resources to lead this project and see to its timely publication.
Stellar Physics and Stellar Types
Stellar Populations and the Interstellar Medium
6
false
false
false
false
false
false
SUPPORTED
STAR
NEUTRON STAR
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J2000
J2000
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STAR
NEUTRON STAR
NO
J2000
J2000
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STAR
NEUTRON STAR
NO
J2000
J2000
F160W (AB) = 21.85
STAR
NEUTRON STAR
NO
J2000
J2000
F160W (AB) = 18.72
STAR
NEUTRON STAR
NO
J2000
J2000
F160W (AB) = 21.03
STAR
NEUTRON STAR
NO
J2000
J2000
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STAR
NEUTRON STAR
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J2000
J2000
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STAR
NEUTRON STAR
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J2000
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STAR
NEUTRON STAR
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J2000
J2000
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STAR
NEUTRON STAR
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J2000
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STAR
NEUTRON STAR
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J2000
J2000
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STAR
NEUTRON STAR
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J2000
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STAR
NEUTRON STAR
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J2000
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STAR
NEUTRON STAR
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J2000
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STAR
NEUTRON STAR
NO
J2000
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WFC3/IR
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)
true
1
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The scheduling data was generated by CASM 33.0.
CASM was run in Phase II mode.
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(Tic-Obset
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(Tic-Orbit
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true
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The scheduling data was generated by CASM 33.0.
CASM was run in Phase II mode.
/private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit12375877789661186625.xml
(Tic-Visit
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(Tic-Obset
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true
1
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The scheduling data was generated by CASM 33.0.
CASM was run in Phase II mode.
/private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit5187304140939417033.xml
(Tic-Visit
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true
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0