- ID:
- ivo://wfau.roe.ac.uk/twomass-dsa
- Title:
- Two Micron All Sky Survey (2MASS)
- Short Name:
- 2MASS
- Date:
- 04 Dec 2019 13:36:55
- Publisher:
- WFAU, Institute for Astronomy, University of Edinburgh
- Description:
- The Two Micron All Sky Survey (2MASS) will provide a uniform survey of the entire sky at three near-infrared wavebands: J(lambdaeff = 1.25 micrometers), H(lambdaeff = 1.65 micrometers), and Ks(lambdaeff = 2.16 micrometers). A major goal of the survey is to probe large scale structures in the Milky Way and in the Local Universe, exploiting the relatively high transparency of the interstellar medium in the near-infrared, and the high near-infrared luminosities of evolved low- and intermediate-mass stars.Home page at http://pegasus.phast.umass.edu/
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/II/108
- Title:
- Two-Micron Sky Survey, Nearest SAO Stars on POSS
- Short Name:
- II/108
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalog is a list of potential guide stars developed for a program to obtain more precise positions of objects in the IRC Two-Micron Sky Survey of Neguebauer and Leighton (1969). For each IRC source (col. 1), it gives: (col. 2) the identification of the star in the SAO catalog which is nearest, (col. 3) the great circle arc distance (in seconds) between the SAO star and the IRC source, (col. 4) the position angle (in degrees) of the IRC source relative to the SAO star, (col. 5) the plate number(s) of the POSS on which the IRC source appears, (col. 6,7) the approximate rectangular coordinates (in mm) of the IRC source on the POSS print area with respect to the Southwest corner, and (col. 8) the modified Luyten Palomar number. The POSS plate numbers given are for the red plates.
22503. Two-Micron Sky Survey (TMSS)
- ID:
- ivo://CDS.VizieR/II/2B
- Title:
- Two-Micron Sky Survey (TMSS)
- Short Name:
- II/2B
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The catalog, giving sources of emission in the 2.2-micrometer region for more than 5000 stars, represents a systematic survey of the Northern Hemisphere for stars brighter than third magnitude. The survey was carried out with a telescope at Mount Wilson, California, having a 62-inch diameter and an f/l aluminized epoxy mirror mounted equatorially. Radiation at an effective wavelength of 2.2 micrometers was detected by a lead sulfide photoconductive cell cooled by liquid nitrogen. In addition to the 2.2-micrometer detector array, radiation at an effective wavelength of 0.84 micrometers was detected by a simple silicon photovoltaic cell. The catalog includes right ascension and declination (B1950.0), K and I magnitudes, number of measurements, V magnitude, spectral types, cross identifications to the numbering systems of the General Catalogue, the Durchmusterung catalogs, the Bright Star Catalogue, and star names.
- ID:
- ivo://CDS.VizieR/J/other/PZ/31.3
- Title:
- Two new cataclysmic variables in Lyra
- Short Name:
- J/other/PZ/31.3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- I report on the discovery of two cataclysmic variables in the same field in Lyra, originally identified on the base of their magnitudes in the USNO-B1.0 catalog and on Palomar images. The historical light curves were analyzed from 300+ photographic plates of the Moscow collection, covering 35 years of observations. One of the two stars, USNO-B1.0 1320-0390658, is showing rather frequent outbursts from B~20 to B=15.2 and is likely a dwarf nova of the UGSS subtype. The other variable, USNO-B1.0 1321-0397655, with only one observed outburst in 1993, from B~19 to I=11.8, is either an UGWZ dwarf nova or a recurrent nova. In both cases, its next outburst can occur in the nearest future.
- ID:
- ivo://CDS.VizieR/J/ApJS/242/4
- Title:
- Two new catalogs of blazar candidates
- Short Name:
- J/ApJS/242/4
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present two catalogs of radio-loud candidate blazars whose Wide-Field Infrared Survey Explorer (WISE) mid-infrared colors are selected to be consistent with the colors of confirmed {gamma}-ray-emitting blazars. The first catalog is the improved and expanded release of the WISE Blazar-like Radio-Loud Sources (WIBRaLS) catalog presented by D'Abrusco et al. It includes sources detected in all four WISE filters, spatially cross-matched with radio sources in one of three radio surveys and radio-loud based on their q_22_ spectral parameter. WIBRaLS2 includes 9541 sources classified as BL Lacs, flat-spectrum radio quasars, or mixed candidates based on their WISE colors. The second catalog, called KDEBLLACS, based on a new selection technique, contains 5579 candidate BL Lacs extracted from the population of WISE sources detected in the first three WISE passbands ([3.4], [4.6], and [12]) only, whose mid-infrared colors are similar to those of confirmed, {gamma}-ray BL Lacs. Members of KDBLLACS are also required to have a radio counterpart and be radio-loud based on the parameter q_12_, defined similarly to the q_22_ used for the WIBRaLS2. We describe the properties of these catalogs and compare them with the largest samples of confirmed and candidate blazars in the literature. We cross-match the two new catalogs with the most recent catalogs of {gamma}-ray sources detected by the Fermi Large Area Telescope. Since spectroscopic observations of candidate blazars from the first WIBRaLS catalog within the uncertainty regions of {gamma}-ray unassociated sources confirmed that ~90% of these candidates are blazars, we anticipate that these new catalogs will again play an important role in the identification of the {gamma}-ray sky.
- ID:
- ivo://CDS.VizieR/J/A+A/621/A110
- Title:
- Two new giant planets around metal-poor stars
- Short Name:
- J/A+A/621/A110
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Statistical studies of exoplanets have shown that giant planets are more commonly hosted by metal-rich dwarf stars than low-metallicity stars, while no such correlation is evident for lower mass planets. The search for giant planets around metal-poor stars and the estimate of their occurrence f_p_ is an important element in providing support to models of planet formation. We present results from the HARPS-N search for giant planets orbiting metal-poor (-1.0<=[Fe/H]<=-0.5dex) stars in the northern hemisphere, complementing a previous HARPS survey on southern stars in order to update the estimate of f_p_. High-precision HARPS-N observations of 42 metal-poor stars were used to search for planetary signals to be fitted using differential evolution Markov chain Monte Carlo single-Keplerian models. We then joined our detections to the results of the previous HARPS survey on 88 metal-poor stars to provide a preliminary estimate of the two-hemisphere f_p_. We report the detection of two new giant planets around HD 220197 and HD 233832. The first companion has Msini=0.20_-0.04_^+0.07^MJup and an orbital period of 1728_-80_^+162^days, and for the second companion, we find two solutions of equal statistical weight with periods of 2058_-40_^+47^ and 4047_-117_^+91^days and minimum masses of 1.78_-0.06_^+0.08^ and 2.72_-0.23_^+0.23^MJup, respectively. Joining our two detections with the three from the southern survey, we obtain a preliminary and conservative estimate of the global frequency of f_p_=3.84_-1.06_^+2.45^% for giant planets around metal-poor stars. The two new giant planets orbit dwarf stars at the metal-rich end of the HARPS-N metal-poor sample. This corroborates previous results that suggested that giant planet frequency is still a rising function of the host star [Fe/H]. We also note that all detections in the overall sample are giant long-period planets.
- ID:
- ivo://CDS.VizieR/J/AJ/159/105
- Title:
- Two new stellar associations in vicinity of the Sun
- Short Name:
- J/AJ/159/105
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this work we report the discovery of two new stellar associations in close vicinity of the Sun at roughly 180 and 150pc. These two associations, u-Tau assoc and e-Tau assoc, were detected based on their clustering in a multi-dimensional parameter space including {alpha}, {delta}, {mu}_{alpha}_, {mu}_{delta}_, and \bar{omega} of Gaia. The fitting of pre-main-sequence model isochrones in their color-magnitude diagrams suggests that the two associations are of about 50Myr old and the group members lower than ~0.8M_{sun}_ are at the stage of post-T Tauri.
- ID:
- ivo://CDS.VizieR/J/ApJ/727/125
- Title:
- Two secondary eclipses of WASP-12b with Spitzer
- Short Name:
- J/ApJ/727/125
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We observed two secondary eclipses of the exoplanet WASP-12b using the Infrared Array Camera on the Spitzer Space Telescope. The close proximity of WASP-12b to its G-type star results in extreme tidal forces capable of inducing apsidal precession with a period as short as a few decades. This precession would be measurable if the orbit had a significant eccentricity, leading to an estimate of the tidal Love number and an assessment of the degree of central concentration in the planetary interior. An initial ground-based secondary-eclipse phase reported by Lopez-Morales et al. (0.510+/-0.002; 2010ApJ...716L..36L) implied eccentricity at the 4.5{sigma} level. The spectroscopic orbit of Hebb et al. (2009ApJ...693.1920H) has eccentricity 0.049+/-0.015, a 3{sigma} result, implying an eclipse phase of 0.509+/-0.007. However, there is a well-documented tendency of spectroscopic data to overestimate small eccentricities. Our eclipse phases are 0.5010+/-0.0006 (3.6 and 5.8um) and 0.5006+/-0.0007 (4.5 and 8.0um). An unlikely orbital precession scenario invoking an alignment of the orbit during the Spitzer observations could have explained this apparent discrepancy, but the final eclipse phase of Lopez-Morales et al. (0.510^+0.007^_-0.006_) is consistent with a circular orbit at better than 2{sigma}. An orbit fit to all the available transit, eclipse, and radial-velocity data indicates precession at <1{sigma}; a non-precessing solution fits better. We also comment on analysis and reporting for Spitzer exoplanet data in light of recent re-analyses.
- ID:
- ivo://CDS.VizieR/J/A+A/627/A43
- Title:
- Two super-Earths orbiting TOI-402
- Short Name:
- J/A+A/627/A43
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Transiting Exoplanet Survey Satellite (TESS) is revolutionising the search for planets orbiting bright and nearby stars. In sectors 3 and 4, TESS observed TOI-402 (TIC-120896927), a bright V=9.1 K1 dwarf also known as HD15337, and found two transiting signals with periods of 4.76 and 17.18 days and radii of 1.90 and 2.21R_{Earth}_, respectively. This star was observed prior to the TESS detection as part of the radial-velocity (RV) search for planets using the HARPS spectrometer, and 85 precise RV measurements were obtained before the launch of TESS over a period of 14 years. In this paper, we analyse the HARPS RV measurements in hand to confirm the planetary nature of these two signals. HD15337 happens to present a stellar activity level similar to the Sun, with a magnetic cycle of similar amplitude and RV measurements that are affected by stellar activity. By modelling this stellar activity in the HARPS radial velocities using a linear dependence with the calcium activity index log(R'_HK_), we are able, with a periodogram approach, to confirm the periods and the planetary nature of TOI-402.01 and TOI-402.02. We then derive robust estimates from the HARPS RVs for the orbital parameters of these two planets by modelling stellar activity with a Gaussian process and using the marginalised posterior probability density functions obtained from our analysis of TESS photometry for the orbital period and time of transit. By modelling TESS photometry and the stellar host characteristics, we find that TOI-402.01 and TOI-402.02 have periods of 4.75642+/-0.00021 and 17.1784+/-0.0016 days and radii of 1.70+/-0.06 and 2.52+/-0.11 (precision 3.6 and 4.2%), respectively. By analysing the HARPS RV measurements, we find that those planets are both super-Earths with masses of 7.20+/-0.81 and 8.79+/-1.68 (precision 11.3 and 19.1%), and small eccentricities compatible with zero at 2{sigma}. Although having rather similar masses, the radii of these two planets are very different, putting them on different sides of the radius gap. By studying the temporal evolution under X-ray and UV (XUV) driven atmospheric escape of the TOI-402 planetary system, we confirm, under the given assumptions, that photo-evaporation is a plausible explanation for this radius difference. Those two planets, being in the same system and therefore being in the same irradiation environment are therefore extremely useful for comparative exoplanetology across the evaporation valley and thus bring constraints on the mechanisms responsible for the radius gap.
- ID:
- ivo://CDS.VizieR/J/AJ/137/3826
- Title:
- Two transits of the giant planet WASP-4b
- Short Name:
- J/AJ/137/3826
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometry of two transits of the giant planet WASP-4b with a photometric precision of 400-800 parts per million and a time sampling of 25-40s. The two midtransit times are determined to within 6s. Together with previously published times, the data are consistent with a constant orbital period, giving no compelling evidence for period variations that would be produced by a satellite or additional planets. Analysis of the new photometry, in combination with stellar-evolutionary modeling, gives a planetary mass and radius of 1.237+/-0.064M_Jup_ and 1.365+/-0.021R_Jup_, respectively. The planet is 15% larger than expected based on previously published models of solar-composition giant planets. With data of the quality presented here, the detection of transits of a "super-Earth" of radius 1.75R_{earth}_ would have been possible.