APASS LANDOLT-SLOAN<i>BVgri</i>PHOTOMETRY OF RAVE STARS. I. DATA, EFFECTIVE TEMPERATURES, AND REDDENINGS

Munari, U.; Henden, A. A.; Frigo, A.; Zwitter, T.; Bienaymé, O.; Bland-Hawthorn, Joss; Boeche, C.; Freeman, K. C.; Gibson, Brad K.; Gilmore, G.; Grebel, Eva K.; Helmi, Amina; Kordopatis, G.; Levine, S. E.; Navarro, Julio F.; Parker, Quentin A.; Reid, Warren A.; Seabroke, G. M.; Siebert, A.; Siviero, A.; Smith, Thomas C.; Steinmetz, Matthias; Templeton, Matthew R.; Terrell, Dirk; Welch, D. L.; Williams, M.; Wyse, Rosemary F. Ġ.

doi:10.1088/0004-6256/148/5/81

Cited by 111 publications

(48 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Similarly to previous studies (Osborn et al 2017;Barros et al 2017;Santerne et al 2018;Lam et al 2018), we used the bayesian software PASTIS (Díaz et al 2014;Santerne et al 2015) to jointly analyse the HARPS radial velocities, the K2 light curve and the spectral energy distribution (SED). For the SED, we used the magnitudes in optical from the APASS survey and in near-infrared from the 2MASS and AllWISE surveys (Henden et al 2015;Munari et al 2014;Cutri & et al 2014). The list of magnitudes is given in Table 1.…”

Section: Pastis Analysismentioning

confidence: 99%

Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS

Lopez

Barros

Santerne

et al. 2019

A&A

View full text Add to dashboard Cite

The detection of low-mass transiting exoplanets in multiple systems brings new constraints to planetary formation and evolution processes and challenges the current planet formation theories. Nevertheless, only a mere fraction of the small planets detected by Kepler and K2 have precise mass measurements, which are mandatory to constrain their composition. We aim to characterise the planets that orbit the relatively bright star K2-138. This system is dynamically particular as it presents the longest chain known to date of planets close to the 3:2 resonance. We obtained 215 HARPS spectra from which we derived the radial-velocity variations of K2-138. Via a joint Bayesian analysis of both the K2 photometry and HARPS radial-velocities (RVs), we constrained the parameters of the six planets in orbit. The masses of the four inner planets, from b to e, are 3.1, 6.3, 7.9, and 13.0 M ⊕ with a precision of 34%, 20%, 18%, and 15%, respectively. The bulk densities are 4.9, 2.8, 3.2, and 1.8 g cm −3 , ranging from Earth to Neptune-like values. For planets f and g, we report upper limits. Finally, we predict transit timing variations of the order two to six minutes from the masses derived. Given its peculiar dynamics, K2-138 is an ideal target for transit timing variation (TTV) measurements from space with the upcoming CHaracterizing ExOPlanet Satellite (CHEOPS) to study this highly-packed system and compare TTV and RV masses.

show abstract

Section: Pastis Analysismentioning

confidence: 99%

Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS

Lopez

Barros

Santerne

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…We have also obtained V -band photometry with the 40cm Bochum Monitoring Telescope (BMT) on Cerro Armazones (Ramolla et al 2013), where the object remained observable longer than from Hawaii. The photometry was calibrated against a set of in-field non-variable stars from the APASS all-sky catalog (Munari et al 2014) and is included as green triangle symbols in Figure 4.…”

Section: Iris Bmt and Ukirtmentioning

confidence: 99%

The New EXor Outburst of ESO-Hα 99 Observed by Gaia ATLAS and TESS

Hodapp¹,

Reipurth²,

Pettersson³

et al. 2019

View full text Add to dashboard Cite

We report photometry and spectroscopy of the outburst of the young stellar object ESO-Hα 99. The outburst was first noticed in Gaia alert Gaia18dvc and later by ATLAS. We have established the outburst light curve with archival ATLAS "Orange" filter photometry, Gaia data, new V -band photometry, and J, H, and K s photometry from IRIS and UKIRT. The brightness has fluctuated several times near the light curve maximum. The TESS satellite observed ESO-Hα 99 with high cadence during one of these minor minima and found brightness fluctuations on timescales of days and hours. Imaging with UKIRT shows the outline of an outflow cavity, and we find one knot of H 2 1−0 S(1) emission, now named MHO 1520, on the symmetry axis of this nebula, indicating recent collimated outflow activity from ESO-Hα 99. Its pre-outburst SED shows a flat FIR spectrum, confirming its early evolutionary state and its similarity to other deeply embedded objects in the broader EXor class. The pre-outburst luminosity is 34 L ⊙ , a much higher luminosity than typical EXors, indicating that ESO-Hα 99 may be a star of intermediate mass.Infrared and optical spectroscopy show a rich emission line spectrum, including H I lines, strong red Ca II emission, as well as infrared CO bandhead emission, all characteristic EXors in the broadest sense. Comparison of the present spectra with an optical spectrum obtained in 1993, presumably in the quiescent state of the object, shows that during the present outburst the continuum component of the spectrum has increased notably more than the emission lines. The Hα equivalent width during the outburst is down to one half of its 1993 level, and shock-excited emission lines are much less prominent. accretion phase, often show substantial variability due to instabilities in the accretion process. The accretion characteristics of young stars have recently been reviewed by Hartmann et al. (2016) and we follow their general line of discussion and the references therein.Traditionally, the photometric outbursts caused by increased accretion rates were divided by Herbig (1977) 2. ESO-Hα 99: CONTEXT AND PRE-OUTBURST PROPERTIES 1

show abstract

“…The IDL 4 (Interactive Data Language) INTERPOL routine was used to interpolate the Sloan r' magnitudes for the three comparison stars from the test observation using published magnitude values (B to K). The comparison stars in the Darksat and STARLINK-1113 observations conducted on 2020/03/06, fortunately have published Sloan g' magnitudes (Munari et al 2014), which allowed a direct calculation of the Darksat and STARLINK-1113 apparent magnitudes in the Sloan g' passband. The details of the comparison stars used in this work, are given in Table 2.…”

Section: Discussionmentioning

confidence: 99%

First observations and magnitude measurement of Starlink’s Darksat

Tregloan-Reed

Otárola

Ortiz

et al. 2020

A&A

View full text Add to dashboard Cite

Aims. Measure the Sloan g' magnitudes of the SpaceX STARLINK-1130 (Darksat) and 1113 LEO communication satellites and determine the effectiveness of the Darksat darkening treatment at 475.4 nm. Methods. Two observations of the SpaceX STARLINK Darksat LEO communication satellite were conducted on 2020/02/08 and 2020/03/06 using a Sloan r' and g' respectively. While a second satellite, STARLINK-1113 was observed on 2020/03/06 using a Sloan g' filter. The initial observation on 2020/02/08 was a test observation when Darksat was still manoeuvring to its nominal orbit and orientation. Based on the successful test observation, the first main observation was conducted on 2020/03/06 along with an observation of a second STARLINK satellite.Results. The calibration, image processing and analysis of the Darksat Sloan g' image gives an estimated Sloan g' magnitude of 7.57 ± 0.04 at a range of 976.50 km. For STARLINK-1113 an estimated Sloan g' magnitude of 6.69 ± 0.05 at a range of 941.62 km was found. When scaled to a range of 550 km, a reduction of (55 % ± 4.8 %) is seen in the reflected solar flux between Darksat and STARLINK-1113. Conclusions. The data and results presented in this work, show that the special darkening "treatment" used by SpaceX for Darksat has reduced the Sloan g' magnitude by 0.88 ± 0.05 mag (55 % ± 4.8 %), when the range is equal to a nominal orbital height (550 km). This result will serve members of the astronomical community modelling the satellite mega-constellations, to ascertain their true impact on both the amateur and professional astronomical communities. Concurrent and further observations are planned to cover the full optical and NIR spectrum, from an ensemble of instruments, telescopes and observatories.

show abstract

APASS LANDOLT-SLOANBVgriPHOTOMETRY OF RAVE STARS. I. DATA, EFFECTIVE TEMPERATURES, AND REDDENINGS

Cited by 111 publications

References 61 publications

Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS

Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS

The New EXor Outburst of ESO-Hα 99 Observed by Gaia ATLAS and TESS

First observations and magnitude measurement of Starlink’s Darksat

Contact Info

Product

Resources

About