The Quick and the Dead: Finding the Surviving Binary Companions of Galactic Supernovae with Gaia

Fraser, M.; Boubert, Douglas

doi:10.3847/1538-4357/aaf6b8

Cited by 21 publications

(19 citation statements)

References 58 publications

(69 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This reduces the number of stars in the cone search. Just as Fraser & Boubert (2019), for Cas A and the Crab Nebula, we did not find any candidates. For SNR G130.7+03.1 (from SN 1181), we found one star with G < 17.0 mag to be consistent with the GC, but it was ruled out due to the missing kinematical consistency with PSR J0205+6449.…”

Section: Discussionsupporting

confidence: 63%

“…Two further candidates are marked, found in Gaia DR2, which are consistent with the Vela pulsar: The star marked in blue was identified by us and could be observed in the near future. The star marked in black was identified by Fraser & Boubert (2019) (hereafter FB19), therein denoted as Star A . It is closer to the nominal past position of the Vela pulsar, but with G = 20.1 mag, it is much too faint to obtain a spectrum with sufficient S / N .…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

A search for runaway stars in 12 Galactic supernova remnants

et al. 2021

View full text Add to dashboard Cite

Runaway stars can result from core-collapse supernovae in multiple stellar systems. If the supernova disrupts the system, the companion is ejected with its former orbital velocity. A clear identification of a runaway star can yield the time and place of the explosion, as well as orbital parameters of the pre-supernova binary system. Previous searches have mostly considered O-and B-type stars as runaway stars because they are always young in absolute terms (not much older than the lifetime of the progenitor) and can be detected up to larger distances. Here, we present a search for runaway stars of all spectral types. For late-type stars, a young age can be inferred from the lithium test. We used Gaia data to identify and characterize runaway star candidates in nearby supernova remnants, obtained spectra of 39 stars with UVES at the VLT and HDS at the Subaru telescope, and found a significant amount of lithium in the spectra of six dwarf stars. We present the spectral analysis, including measurements of radial velocities, atmospheric parameters, and lithium abundances. Then, we estimate the ages of our targets from the Hertzsprung-Russell diagram and, using the lithium test, present a selection of promising runaway star candidates and draw constraints on the number of ejected runaway stars compared to model expectations.

show abstract

Section: Discussionsupporting

confidence: 63%

Section: Discussionmentioning

confidence: 99%

A search for runaway stars in 12 Galactic supernova remnants

et al. 2021

View full text Add to dashboard Cite

show abstract

“…The commonly used value for the distance to the Crab is 2 kpc (Trimble 1968). However, a Gaia measurement of the pulsar's parallax (Fraser & Boubert 2019) gives a larger distance of 3.37 +4.04 −0.97 kpc. We use the Trimble (1968) distance for consistency with previous work -using the larger distance would increase all dust masses by a factor of ∼2.8.…”

Section: Dust Speciesmentioning

confidence: 96%

Dust masses and grain size distributions of a sample of Galactic pulsar wind nebulae

Priestley

Barlow

Chawner

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We calculate dust spectral energy distributions (SEDs) for a range of grain sizes and compositions, using physical properties appropriate for five pulsar wind nebulae (PWNe) from which dust emission associated with the ejecta has been detected. By fitting the observed dust SED with our models, with the number of grains of different sizes as the free parameters, we are able to determine the grain size distribution and total dust mass in each PWN. We find that all five PWNe require large ($\ge 0.1 \, {\rm \mu m}$) grains to make up the majority of the dust mass, with strong evidence for the presence of micron-sized or larger grains. Only two PWNe contain non-negligible quantities of small ($\lt 0.01 \, {\rm \mu m}$) grains. The size distributions are generally well-represented by broken power laws, although our uncertainties are too large to rule out alternative shapes. We find a total dust mass of $0.02\rm {-}0.28 \, {\rm M}_\odot$ for the Crab Nebula, depending on the composition and distance from the synchrotron source, in agreement with recent estimates. For three objects in our sample, the PWN synchrotron luminosity is insufficient to power the observed dust emission, and additional collisional heating is required, either from warm, dense gas as found in the Crab Nebula, or higher temperature shocked material. For G54.1+0.3, the dust is heated by nearby OB stars rather than the PWN. Inferred dust masses vary significantly depending on the details of the assumed heating mechanism, but in all cases large mass fractions of micron-sized grains are required.

show abstract

“…The total (warm+cold) dust masses are summarised in Column 8 (assuming a distance to the Crab of D=2 kpc). These dust masses could go up by a factor of 2.8 based on the revised distance estimate for the Crab inferred from GAIA data (Fraser & Boubert 2019). The maximum expected dust masses for different grain species are provided in Column 9 based on a condensation efficiency of 100% and the estimated yields from nucleosynthesis models from Woosley & Weaver (1995) for a progenitor mass of 11 M .…”

Section: Resolved Modelling Of the Crab Nebulamentioning

confidence: 99%

“…This distance measurement to the Crab is quite uncertain, and a recent GAIA study of the central pulsar has suggested that the distance to the Crab might be underestimated(Fraser & Boubert 2019). However, since this GAIA measurement is also quite uncertain we adopt in this paper the canonical distance of 2 kpc, which has most commonly been used.…”

mentioning

confidence: 99%

The dust content of the Crab Nebula

Looze

Barlow

Bandiera

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We have modelled the near-infrared to radio images of the Crab Nebula with a Bayesian SED model to simultaneously fit its synchrotron, interstellar and supernova dust emission. We infer an interstellar dust extinction map with an average A V = 1.08 ± 0.38 mag, consistent with a small contribution ( 22%) to the Crab's overall infrared emission. The Crab's supernova dust mass is estimated to be between 0.032 and 0.049 M (for amorphous carbon grains) with an average dust temperature T dust =41±3 K, corresponding to a dust condensation efficiency of 8-12%. This revised dust mass is up to an order of magnitude lower than some previous estimates, which can be attributed to our different interstellar dust corrections, lower SPIRE flux densities, and higher dust temperatures than were used in previous studies. The dust within the Crab is predominantly found in dense filaments south of the pulsar, with an average V band dust extinction of A V = 0.20 − 0.39 mag, consistent with recent optical dust extinction studies. The modelled synchrotron power-law spectrum is consistent with a radio spectral index α radio =0.297±0.009 and an infrared spectral index α IR =0.429±0.021. We have identified a millimetre excess emission in the Crab's central regions, and argue that it most likely results from two distinct populations of synchrotron emitting particles. We conclude that the Crab's efficient dust condensation (8-12%) provides further evidence for a scenario where supernovae can provide substantial contributions to the interstellar dust budgets in galaxies.

show abstract

The Quick and the Dead: Finding the Surviving Binary Companions of Galactic Supernovae with Gaia

Cited by 21 publications

References 58 publications

A search for runaway stars in 12 Galactic supernova remnants

A search for runaway stars in 12 Galactic supernova remnants

Dust masses and grain size distributions of a sample of Galactic pulsar wind nebulae

The dust content of the Crab Nebula

Contact Info

Product

Resources

About