- ID:
- ivo://CDS.VizieR/J/AJ/161/54
- Title:
- VRI photometry of MOA 2009-BLG-319
- Short Name:
- J/AJ/161/54
- Date:
- 10 Dec 2021
- Publisher:
- CDS
- Description:
- We present an adaptive optics (AO) analysis of images from the KeckII telescope NIRC2 instrument of the planetary microlensing event MOA-2009-BLG-319. The ~10yr baseline between the event and the Keck observations allows the planetary host star to be detected at a separation of 66.5{+/-}1.7mas from the source star, consistent with the light-curve model prediction. The combination of the host star brightness and light-curve parameters yields host star and planet masses of M_host_=0.524{+/-}0.048M{sun} and m_p_=67.3{+/-}6.2M{Earth} at a distance of DL=7.1{+/-}0.7kpc. The star-planet projected separation is 2.03{+/-}0.21au. The planet-to-star mass ratio of this system, q=(3.857{+/-}0.029)x10^-4^, places it in the predicted "planet desert" at 10^-4^<q<4x10^-4^ according to the runaway gas accretion scenario of the core accretion theory. Seven of the 30 planets in the Suzuki et al. sample fall in this mass ratio range, and this is the third with a measured host mass. All three of these host stars have masses of 0.5<~M_host_/M{sun}<~0.7, which implies that this predicted mass ratio gap is filled with planets that have host stars within a factor of two of 1M{sun}. This suggests that runaway gas accretion does not play a major role in determining giant planet masses for stars somewhat less massive than the Sun. Our analysis has been accomplished with a modified DAOPHOT code that has been designed to measure the brightness and positions of closely blended stars. This will aid in the development of the primary method that the Nancy Grace Roman Space Telescope mission will use to determine the masses of microlens planets and their hosts.
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- ID:
- ivo://CDS.VizieR/J/AJ/120/1
- Title:
- VRI photometry of PDCS survey
- Short Name:
- J/AJ/120/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper presents the COP (CFHT optical PDCS; CFHT: Canada-France-Hawaii Telescope, PDCS: Palomar Distant Cluster Survey) survey data. We describe our photometric and spectroscopic observations with the multiobject spectrograph (MOS) at the CFHT. A comparison of the photometry from the PDCS catalogs and from the new images we have obtained at the CFHT shows that the different magnitude systems can be cross-calibrated. After identification between the PDCS catalogs and our new images, we built catalogs with redshift, coordinates, and V_PDCS_, I_PDCS_, and R_COP_ magnitudes. We have classified the galaxies along the lines of sight into field and structure galaxies using a gap technique from Katgert et al. In total we have observed 18 significant structures along the 10 lines of sight.
- ID:
- ivo://CDS.VizieR/J/AJ/127/2228
- Title:
- VRI photometry of PMS stars in NGC 2264 OB
- Short Name:
- J/AJ/127/2228
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We summarize the results of an observing campaign to identify periodic pre-main-sequence (PMS) variables in the NGC 2264 OB association. We find 201 periodic candidates.
- ID:
- ivo://CDS.VizieR/J/MNRAS/369/697
- Title:
- VRI photometry of SMC/LMC globular clusters
- Short Name:
- J/MNRAS/369/697
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present accurate integrated-light photometry in Johnson/Cousins V, R and I for a sample of 28 globular clusters in the Magellanic Clouds. The majority of the clusters in our sample have reliable age and metallicity estimates available in the literature. The sample encompasses ages between 50Myr and 7Gyr, and metallicities ([Fe/H]) between 1.5 and 0.0dex. The sample is dominated by clusters of ages between roughly 0.5 and 2Gyr, an age range during which the bolometric luminosity of simple stellar populations is dominated by evolved red giant branch stars and thermally pulsing asymptotic giant branch (TP-AGB) stars whose theoretical colours are rather uncertain. The VRI colours presented in this paper have been used to calibrate stellar population synthesis model predictions.
- ID:
- ivo://CDS.VizieR/J/A+AS/116/403
- Title:
- VRI photometry of stars in 12 BL Lac objects
- Short Name:
- J/A+AS/116/403
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present VR_cI_c Johnson-Cousins magnitudes of field comparison stars for twelve BL Lacertae objects belonging to the more large sample of blazars which is monitored at Perugia Astronomical Observatory. These comparison stars can be used in the long-term CCD photometric monitoring of BL Lac objects aimed to understand the characteristics of their variability. Finding charts for all of these comparison sequences are also included in this paper. For a description of the (RI)c photometric system, see e.g. the General Catalog of Photometric Data <GCPD/54>
- ID:
- ivo://CDS.VizieR/J/AJ/130/2252
- Title:
- VRI photometry of V410 Aur
- Short Name:
- J/AJ/130/2252
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The complete charge-coupled device (CCD) light curves in the V, R, and I bands for the eclipsing binary V410 Aur were observed at the Yunnan Observatory in China.
- ID:
- ivo://CDS.VizieR/J/A+A/639/L10
- Title:
- VRI photometry of V392 Per
- Short Name:
- J/A+A/639/L10
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Nova Per 2018 (= V392 Per) halted the decline from maximum when it was 2mag brighter than quiescence and since 2019 has been stable at such a plateau. The ejecta have already fully diluted into the interstellar space. We obtained BVRIgrizY photometry and optical spectroscopy of V392 Per during the plateau phase and compared it with equivalent data gathered prior to the nova outburst. We find the companion star (CS) to be a G9 IV/III and the orbital period to be 3.4118 days, making V392 Per the longest known period for a classical nova. The location of V392 Per on the theoretical isochrones is intermediate between that of classical novae and novae erupting within symbiotic binaries, in a sense bridging the gap. The reddening is derived to be E(B-V)=0.72 and the fitting to isochrones returns a 3.6Gyr age for the system and 1.35M_{sun}_, 5.3R_{sun}_, and 15L_{sun}_ for the companion. The huge Ne overabundance in the ejecta and the very fast decline from nova maximum both point to a massive white dwarf (M(WD)>=1.1/1.2M_{sun}_). The system is viewed close to pole-on conditions and the current plateau phase is caused by irradiation of the CS by the WD still burning at the surface.
- ID:
- ivo://CDS.VizieR/J/A+AS/112/291
- Title:
- VRI photometry of wide double stars
- Short Name:
- J/A+AS/112/291
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We are presenting VRI photometry of 93 wide visual double stars having late B- or A- type primaries, taken from the Annex of Double and Multiple Stars of the HIPPARCOS Input Catalogue. Spectral types have been estimated for most of the primaries and for the majority of the secondaries. 40% of them probably have common origin components, for which we calculated photometric parallaxes and some orbital values estimates.
- ID:
- ivo://CDS.VizieR/J/ApJS/242/15
- Title:
- VRI photometry & taxonomy for >~2000 MBAs
- Short Name:
- J/ApJS/242/15
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present here multiband photometry for over 2000 Main-Belt asteroids. For each target, we report the probabilistic taxonomy using the measured V-R and V-I colors in combination with a machine-learning-generated decision surface in color-color space. Through this method, we classify >85% of our targets as one the four main Bus-DeMeo complexes: S-, C-, X-, or D-type. Roughly one-third of our targets have a known associated dynamic family, with 69 families represented in our data. Within uncertainties, our results show no discernible difference in taxonomic distribution between family members and non-family members. Nine of the sixty-nine families represented in our observed sample had 20 or more members present, and therefore, we investigate the taxonomy of these families in more detail and find excellent agreement with the literature. Out of these nine well-sampled families, our data show that the Themis, Koronis, Hygiea, Massalia, and Eunomia families display a high degree of taxonomic homogeneity and that the Vesta, Flora, Nysa-Polana, and Eos families show a significant level of mixture in taxonomies. Using the taxonomic purity and the degree of dispersion in observed colors for each of the nine well-sampled collisional families, we also speculate which of these families potentially originated from a differentiated parent body and/or is a family with a possible undetermined nested family. In addition, we obtained sufficient photometric data for 433 of our targets to extract reliable rotation periods and observe no obvious correlation between rotation properties and family membership.
- ID:
- ivo://CDS.VizieR/J/AJ/143/122
- Title:
- VR light curves of CK Boo
- Short Name:
- J/AJ/143/122
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present precision CCD photometry, a period study, and a two-color simultaneous Wilson code solution of the short-period contact binary CK Bootis. The asymmetric light curves were modeled by a dark spot on the primary component. The result identifies that CK Boo is an A-type W UMa binary with a high fillout of f=71.7(+/-4.4)%. From the O-C curve, it is found that the orbital period changes in a complicated mode, i.e., a long-term increase with two sinusoidal variations. One cyclic oscillation with a period of 10.67(+/-0.20)yr may result from magnetic activity cycles, which are identified by the variability of Max. I-Max. II. Another sinusoidal variation (i.e., A=0.0131days(+/-0.0009days) and P3=24.16(+/-0.64)yr) may be attributed to the light-time effect due to a third body. This kind of additional companion can extract angular momentum from the central binary system. The orbital period secularly increases at a rate of dP/dt=+9.79(+/-0.80)*10^-8days/yr, which may be interpreted by conservative mass transfer from the secondary to the primary. This kind of deep, low-mass ratio overcontact binaries may evolve into a rapid-rotating single star, only if the contact configuration do not break down at J_spin_>(1/3)J_orb_.
