Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

Campbell, H.; Marsh, T. R.; Fraser, M.; Hodgkin, S. T.; Miguel, Enrique de; Gänsicke, B. T.; Steeghs, D.; Hourihane, A.; Breedt, E.; Littlefair, S. P.; Koposov, S. E.; Wyrzykowski, Ł.; Altavilla, G.; Blagorodnova, N.; Clementini, G.; Damljanović, G.; Delgado, A.; Dennefeld, M.; Drake, A. J.; Fernández-Hernández, J.; Gilmore, G.; Gualandi, R.; Hamanowicz, A.; Handzlik, Barbara; Hardy, L. K.; Harrison, D. L.; Iłkiewicz, Krystian; Jonker, P. G.; Kochanek, C. S.; Kołaczkowski, Z.; Kostrzewa-Rutkowska, Z.; Kotak, R.; Leeuwen, G. van; Leto, G.; Ochner, P.; Pawlak, M.; Palaversa, L.; Rixon, G.; Rybicki, K.; Shappee, B. J.; Smartt, S. J.; Torres, M. A. P.; Tomasella, L.; Turatto, M.; Ulaczyk, K.; Velzen, S. van; Vince, O.; Walton, N. A.; Wielgórski, Piotr; Wevers, T.; Whitelock, P. A.; Yoldaş, A.; Angeli, F. De; Burgess, P.; Busso, G.; Busuttil, R.; Butterley, T.; Chambers, K.; Copperwheat, C. M.; Danilet, A. B.; Dhillon, V. S.; Evans, D. W.; Eyer, L.; Froebrich, D.; Gomboc, A.; Holland, G.; Holoien, T. W. S.; Jarvis, J. F.; Kaiser, Nick; Канн, Д. А.; Koester, D.; Kolb, U.; Komossa, S.; Magnier, E. A.; Mahabal, A.; Polshaw, J.; Prieto, J. L.; Prusti, T.; Riello, M.; Scholz, Alexander; Simonian, G.; Stanek, K. Z.; Szabados, László; Waters, C.; Wilson, Richard W.

doi:10.1093/mnras/stv1224

Cited by 41 publications

(41 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The candidate transients are then filtered and the most interesting candidates are published as alerts, including the relevant Gaia data to enable rapid follow-up with ground-based telescopes. The science alerts system has been tested during an extended validation campaign (leading, for example, to the discovery of an eclipsing AM CVn system; Campbell et al 2015), and is now routinely producing alerts that can be accessed through http://gsaweb.ast.cam.ac.uk/alerts Solar system alerts. This system processes the daily IDT outputs to search for new solar system objects (mostly main-belt asteroids and near-Earth objects) that can be recognised by their fast motion across the sky (a typical main-belt asteroid moves at ∼10 mas s −1 with respect to the stars; Tanga et al 2016).…”

Section: Daily Data Processingmentioning

confidence: 99%

TheGaiamission

Prusti¹,

Bruijne²,

Brown³

et al. 2016

A&A

Self Cite

5,308

1,139

View full text Add to dashboard Cite

Gaia is a cornerstone mission in the science programme of the European Space Agency (ESA). The spacecraft construction was approved in 2006, following a study in which the original interferometric concept was changed to a direct-imaging approach. Both the spacecraft and the payload were built by European industry. The involvement of the scientific community focusses on data processing for which the international Gaia Data Processing and Analysis Consortium (DPAC) was selected in 2007. Gaia was launched on 19 December 2013 and arrived at its operating point, the second Lagrange point of the Sun-Earth-Moon system, a few weeks later. The commissioning of the spacecraft and payload was completed on 19 July 2014. The nominal five-year mission started with four weeks of special, ecliptic-pole scanning and subsequently transferred into full-sky scanning mode. We recall the scientific goals of Gaia and give a description of the as-built spacecraft that is currently (mid-2016) being operated to achieve these goals. We pay special attention to the payload module, the performance of which is closely related to the scientific performance of the mission. We provide a summary of the commissioning activities and findings, followed by a description of the routine operational mode. We summarise scientific performance estimates on the basis of in-orbit operations. Several intermediate Gaia data releases are planned and the data can be retrieved from the Gaia Archive, which is available through the Gaia home page.

show abstract

Section: Daily Data Processingmentioning

confidence: 99%

TheGaiamission

Prusti¹,

Bruijne²,

Brown³

et al. 2016

A&A

Self Cite

5,308

1,139

View full text Add to dashboard Cite

show abstract

“…8. Although Gaia DR1 is the first major catalogue release with results from the Gaia mission, Gaia data has already been made publicly available as "Science Alerts" on transient sources, which for example led to the discovery of only the third known eclipsing AM CVn-system (Campbell et al 2015).…”

Section: Introductionmentioning

confidence: 99%

GaiaData Release 1

Brown¹,

Vallenari²,

Prusti³

et al. 2016

A&A

Self Cite

1,715

272

View full text Add to dashboard Cite

Context. At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7. Aims. A summary of Gaia DR1 is presented along with illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release. Methods. The raw data collected by Gaia during the first 14 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into an astrometric and photometric catalogue. Results. Gaia DR1 consists of three components: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the Hipparcos and Tycho-2 catalogues -a realisation of the Tycho-Gaia Astrometric Solution (TGAS) -and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set, consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of ∼3000 Cepheid and RR Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas yr −1 for the proper motions. A systematic component of ∼0.3 mas should be added to the parallax uncertainties. For the subset of ∼94 000 Hipparcos stars in the primary data set, the proper motions are much more precise at about 0.06 mas yr −1 . For the secondary astrometric data set, the typical uncertainty of the positions is ∼10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to ∼0.03 mag over the magnitude range 5 to 20.7. Conclusions. Gaia DR1 is an important milestone ahead of the next Gaia data release, which will feature five-parameter astrometry for all sources. Extensive validation shows that Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data.

show abstract

“…Only three eclipsing AM CVns have been discovered to date: PTF1J1919+4815, in which just the edge of the disc and bright spot are eclipsed (Levitan et al 2014); YZ LMi (also known as SDSS J092638.71+362402.4), in which the white dwarf is partially eclipsed (Anderson et al 2005;Copperwheat et al 2011); and Gaia14aae (also known as ASASSN-14cn), the only known AM CVn in which the white dwarf is fully eclipsed (Campbell et al 2015). Due to their eclipsing nature, the latter two of these systems are ideal targets for parameter studies.…”

mentioning

confidence: 99%

High-speed photometry of Gaia14aae: an eclipsing AM CVn that challenges formation models

Green

Marsh

Steeghs

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

AM CVn-type systems are ultra-compact, hydrogen-deficient accreting binaries with degenerate or semi-degenerate donors. The evolutionary history of these systems can be explored by constraining the properties of their donor stars. We present high-speed photometry of Gaia14aae, an AM CVn with a binary period of 49.7 minutes and the first AM CVn in which the central white dwarf is fully eclipsed by the donor star. Modelling of the lightcurves of this system allows for the most precise measurement to date of the donor mass of an AM CVn, and relies only on geometric and well-tested physical assumptions. We find a mass ratio q = M 2 /M 1 = 0.0287 ± 0.0020 and masses M 1 = 0.87 ± 0.02M and M 2 = 0.0250 ± 0.0013M . We compare these properties to the three proposed channels for AM CVn formation. Our measured donor mass and radius do not fit with the contraction that is predicted for AM CVn donors descended from white dwarfs or helium stars at long orbital periods. The donor properties we measure fall in a region of parameter space in which systems evolved from hydrogen-dominated cataclysmic variables are expected, but such systems should show spectroscopic hydrogen, which is not seen in Gaia14aae. The evolutionary history of this system is therefore not clear. We consider a helium-burning star or an evolved cataclysmic variable to be the most likely progenitors, but both models require additional processes and/or finetuning to fit the data. Additionally, we calculate an updated ephemeris which corrects for an anomalous time measurement in the previously published ephemeris.

show abstract

Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

Cited by 41 publications

References 48 publications

TheGaiamission

TheGaiamission

GaiaData Release 1

High-speed photometry of Gaia14aae: an eclipsing AM CVn that challenges formation models

Contact Info

Product

Resources

About