Supernovae and Gaia

Altavilla, G.; Botticella, M. T.; Turatto, M.

doi:10.1007/s10509-012-1017-6

Cited by 18 publications

(23 citation statements)

References 130 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our prediction for the numbers of all types of SNe detected with Gaia agree with the numbers reported in previous works (Belokurov & Evans 2003;Altavilla et al 2012). Belokurov & Evans (2003) also assumed SN rates to be a function of galaxy type and luminosity.…”

Section: Comparison With Literaturesupporting

confidence: 90%

Gaiatransient detection efficiency: hunting for nuclear transients

Blagorodnova

Velzen

Harrison

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present a study of the detectability of transient events associated with galaxies for the Gaia European Space Agency astrometric mission. We simulated the on-board detections, and on-ground processing for a mock galaxy catalogue to establish the properties required for the discovery of transient events by Gaia, specifically tidal disruption events (TDEs) and supernovae (SNe). Transients may either be discovered by the on-board detection of a new source or by the brightening of a previously known source. We show that Gaia transients can be identified as new detections on-board for offsets from the host galaxy nucleus of 0.1-0.5 arcsec, depending on magnitude and scanning angle. The Gaia detection system shows no significant loss of SNe at close radial distances to the nucleus. We used the detection efficiencies to predict the number of transients events discovered by Gaia. For a limiting magnitude of 19, we expect around 1300 SNe per year: 65% SN Ia, 28% SN II and 7% SN Ibc, and ∼20 TDEs per year.

show abstract

Section: Comparison With Literaturesupporting

confidence: 90%

Gaiatransient detection efficiency: hunting for nuclear transients

Blagorodnova

Velzen

Harrison

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…Our own simulations (in agreement with [5]) suggest that we will detect 15 000 supernovae (SN) during the lifetime of Gaia down to G = 20. For SN Ia, Ib/c and IIL, we catch 30-40% of them on the rise; for type IIP, it is closer to 10 per cent.…”

Section: Supernovaesupporting

confidence: 85%

Transient astronomy with the Gaia satellite

Hodgkin

Wyrzykowski

Blagorodnova

et al. 2013

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

Gaia is a cornerstone European Space Agency astrometry space mission and a successor to the Hipparcos mission. Gaia will observe the whole sky for 5 years, providing a serendipitous opportunity for the discovery of large numbers of transient and anomalous events, e.g. supernovae, novae and microlensing events, gamma-ray burst afterglows, fallback supernovae, as well as theoretical or unexpected phenomena. In this paper, we discuss our preparations to use Gaia to search for transients at optical wavelengths, and briefly describe the early detection, classification and prompt publication of anomalous sources.

show abstract

“…Gaia will observe not only stars, but also tens of thousands of quasars, unresolved galaxies, Solar system objects, many transient and variable objects like supernovae, and finally the interstellar medium (Altavilla et al 2012;Ducourant et al 2014;Eyer et al 2014;de Bruijne et al 2015;Proft & Wambsganss 2015;Zwitter & Kos 2015;Bachchan, Hobbs, & Lindegren 2016;Tanga et al 2016). Gaia will also pose a challenge because of its data amount and complexity, pushing the astrophysical community farther into the path of big data and data mining (Gaia Collaboration 2016a).…”

Section: Introductionmentioning

confidence: 99%

Globular clusters with Gaia

Pancino

Bellazzini

Giuffrida

et al. 2017

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The treatment of crowded fields in Gaia data will only be a reality in a few years from now. In particular, for globular clusters, only the end-of-mission data (public in 2022-2023) will have the necessary full crowding treatment and will reach sufficient quality for the faintest stars. As a consequence, the work on the deblending and decontamination pipelines is still ongoing. We describe the present status of the pipelines for different Gaia instruments, and we model the end-of-mission crowding errors on the basis of available information. We then apply the nominal post-launch Gaia performances, appropriately worsened by the estimated crowding errors, to a set of 18 simulated globular clusters with different concentration, distance, and field contamination. We conclude that there will be 10 3 -10 4 stars with astrometric performances virtually untouched by crowding (contaminated by <1 mmag) in the majoritiy of clusters. The most limiting factor will be field crowding, not cluster crowding: the most contaminated clusters will only contain 10-100 clean stars. We also conclude that: (i) the systemic proper motions and parallaxes will be determined to 1% or better up to 15 kpc, and the nearby clusters will have radial velocities to a few km s −1 ; (ii) internal kinematics will be of unprecendented quality, cluster masses will be determined to 10% up to 15 kpc and beyond, and it will be possible to identify differences of a few km s −1 or less in the kinematics (if any) of cluster sub-populations up to 10 kpc and beyond; (iii) the brightest stars (V 17 mag) will have space-quality, wide-field photometry (mmag errors), and all Gaia photometry will have 1-3% errors on the absolute photometric calibration.

show abstract

Supernovae and Gaia

Cited by 18 publications

References 130 publications

Gaiatransient detection efficiency: hunting for nuclear transients

Gaiatransient detection efficiency: hunting for nuclear transients

Transient astronomy with the Gaia satellite

Globular clusters with Gaia

Contact Info

Product

Resources

About