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361. 100-Micron Survey of the Galactic Plane
ID:
ivo://CDS.VizieR/II/56
Title:
100-Micron Survey of the Galactic Plane
Short Name:
II/56
Date:
21 Oct 2021
Publisher:
CDS
Description:
The catalog represents a survey of a portion of the galactic plane at a wavelength of 100 micrometers with a balloon-borne, stabilized, 12-inch infrared telescope having a sensitivity of 10(-22) W/m2/Hz. The survey covers 750 square degrees of the sky, including most of the galactic plane between galactic longitudes of 335 and 88 degrees, plus a number of other selected areas of interest. Seventy-two sources have been detected, 60 of which are identified with continuum radio sources, bright nebulae, dark nebulae, and infrared stars. The catalog includes right ascension and declination (B1950.0), galactic coordinates, 100-micrometer peak flux densities, sizes of sources, and identifications.
362. Mid-IR content of BGPS sources
ID:
ivo://CDS.VizieR/J/ApJ/731/90
Title:
Mid-IR content of BGPS sources
Short Name:
J/ApJ/731/90
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the results of a search for mid-infrared signs of star formation activity in the 1.1mm sources in the Bolocam Galactic Plane Survey (BGPS). We have correlated the BGPS catalog (Cat. J/ApJS/188/123) with available mid-IR Galactic plane catalogs based on the Spitzer Space Telescope GLIMPSE legacy survey (including Cat. J/AJ/136/2413 and the EGO cat. J/AJ/136/2391) and the Midcourse Space Experiment (MSX) Galactic plane survey (RMS catalog, Hoare et al. 2004ASPC..317..156H). We find that 44% (3712 of 8358) of the BGPS sources contain at least one mid-IR source, including 2457 of 5067 (49%) within the area where all surveys overlap (10{deg}<l<65{deg}). Accounting for chance alignments between the BGPS and mid-IR sources, we conservatively estimate that 20% of the BPGS sources within the area where all surveys overlap show signs of active star formation. We separate the BGPS sources into four groups based on their probability of star formation activity. Extended Green Objects and Red MSX Sources make up the highest probability group, while the lowest probability group is comprised of "starless" BGPS sources which were not matched to any mid-IR sources. The mean 1.1mm flux of each group increases with increasing probability of active star formation.
363. Milky Way Age-Metallicity-orbital energy relation
ID:
ivo://CDS.VizieR/J/AJ/162/42
Title:
Milky Way Age-Metallicity-orbital energy relation
Short Name:
J/AJ/162/42
Date:
21 Mar 2022 00:01:52
Publisher:
CDS
Description:
Globular clusters can form inside their host galaxies at high redshift when gas densities are higher and gas-rich mergers are common. They can also form inside lower-mass galaxies that have since been accreted and tidally disrupted, leaving their globular cluster complement bound to higher-mass halos. We argue that the age-metallicity-specific orbital energy relation in a galaxy's globular cluster system can be used to identify its origin. Gas-rich mergers should produce tightly bound systems in which metal-rich clusters are younger than metal-poor clusters. Globular clusters formed in massive disks and then scattered into a halo should have no relationship between age and specific orbital energy. Accreted globular clusters should produce weakly bound systems in which age and metallicity are correlated with eachother but inversely correlated with specific orbital energy. We use precise relative ages, self-consistent metallicities, and space-based proper motion-informed orbits to show that the Milky Way's metal-poor globular cluster system lies in a plane in age-metallicity-specific orbital energy space. We find that relatively young or metal-poor globular clusters are weakly bound to the Milky Way, while relatively old or metal-rich globular clusters are tightly bound to the Galaxy. While metal-rich globular clusters may be formed either in situ or ex situ, our results suggest that metal-poor clusters are formed outside of the Milky Way in now-disrupted dwarf galaxies. We predict that this relationship between age, metallicity, and specific orbital energy in a L* galaxy's globular cluster system is a natural outcome of galaxy formation in a {Lambda}CDM universe.
364. Milky way and stellar distributions
ID:
ivo://CDS.VizieR/J/AJ/118/895
Title:
Milky way and stellar distributions
Short Name:
J/AJ/118/895
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the results of a photometric and spectroscopic study of stars in four fields toward the inner disk and Galactic bulge. The fields are located symmetrically about the minor axis of the Milky Way at (l, b)=(-24.8{deg}, -6.0{deg}), (-8.7{deg}, -6.0{deg}), (+8.4{deg}, -6.0{deg}), and (+24.4{deg}, -6.1{deg}). We measured radial velocities and strengths of selected absorption-line indexes and derived the average reddening to each field, individual metallicities and photometric parallaxes for each star, and mean azimuthal rotation velocities and velocity dispersions for each field.
365. Milky Way Cepheids radial velocities
ID:
ivo://CDS.VizieR/J/A+A/534/A94
Title:
Milky Way Cepheids radial velocities
Short Name:
J/A+A/534/A94
Date:
21 Oct 2021
Publisher:
CDS
Description:
We determine Period-Luminosity relations for Milky Way Cepheids in the optical and near-IR bands. These relations can be used directly as reference for extra-galactic distance determination to Cepheid populations with solar metallicity, and they form the basis for a direct comparison with relations obtained in exactly the same manner for stars in the Magellanic Clouds, presented in an accompanying paper. In that paper we show that the metallicity effect is very small and consistent with a null effect, particularly in the near-IR bands, and we combine here all 111 Cepheids from the Milky Way, the LMC and SMC to form a best relation. We employ the near-IR surface brightness (IRSB) method to determine direct distances to the individual Cepheids after we have recalibrated the projection factor using the recent parallax measurements to ten Galactic Cepheids and the constraint that Cepheid distances to the LMC should be independent of pulsation period. We confirm our earlier finding that the projection factor for converting radial velocity to pulsational velocity depends quite steeply on pulsation period, p=1.550-0.186*log(P) in disagrement with recent theoretical predictions. We find PL relations based on 70 Milky Way fundamental mode Cepheids of Mk=-3.33(+/-0.09)(log(P)-1.0)-5.66(+/-0.03), Wvi=-3.26(+/-0.11)(log(P)-1.0)-5.96(+/-0.04). Combining the 70 Cepheids presented here with the results for 41 Magellanic Cloud Cepheids which are presented in an accompanying paper, we find Mk=-3.30(+/-0.06)(log(P)-1.0)-5.65(+/-0.02), Wvi=-3.32(+/-0.08)(log(P)-1.0)-5.92(+/-0.03). We delineate the Cepheid PL relation using 111 Cepheids with direct distances from the IRSB analysis. The relations are by construction in agreement with the recent HST parallax distances to Cepheids and slopes are in excellent agreement with the slopes of apparent magnitudes versus period observed in the LMC.
366. Milky Way detached double-lined EB catalog
ID:
ivo://CDS.VizieR/J/other/PASA/31.24
Title:
Milky Way detached double-lined EB catalog
Short Name:
J/other/PASA/31.
Date:
21 Oct 2021
Publisher:
CDS
Description:
The most accurate stellar astrophysical parameters were collected from the solutions of the light and the radial velocity curves of 257 detached double-lined eclipsing binaries in the Milky Way. The catalogue contains masses, radii, surface gravities, effective temperatures, luminosities, projected rotational velocities of the component stars, and the orbital parameters. The number of stars with accurate parameters increased 67% in comparison to the most recent similar collection by Torres, Andersen, & Gimenez (2010, Cat. J/other/A+ARv/18.67). Distributions of some basic parameters were investigated. The ranges of effective temperatures, masses, and radii are (K)<43000, 0.18<M/M_{sun}_<33, and 0.2<R/R_{sun}_<21.2, respectively. Being mostly located in one kpc in the Solar neighborhood, the present sample covers distances up to 4.6kpc within the two local Galactic arms, Carina-Sagittarius and Orion Spur. The number of stars with both mass and radius measurements better than 1% uncertainty is 93, better than 3% uncertainty is 311, and better than 5% uncertainty is 388. It is estimated from the Roche lobe filling factors that 455 stars (88.5% of the sample) are spherical within 1% of uncertainty.
367. Milky Way disk kinematic sub-structures
ID:
ivo://CDS.VizieR/J/A+A/619/A72
Title:
Milky Way disk kinematic sub-structures
Short Name:
J/A+A/619/A72
Date:
21 Oct 2021
Publisher:
CDS
Description:
Gaia DR2 has delivered full-sky six-dimensional measurements for millions of stars, and the quest to understand the dynamics of our Galaxy has entered a new phase. Our aim is to reveal and characterise the kinematic substructure of the different Galactic neighbourhoods, to form a picture of their spatial evolution that can be used to infer the Galactic potential, its evolution, and its components. We take approximately 5 million stars in the Galactic disk from the Gaia DR2 catalogue and build the velocity distribution in different Galactic neighbourhoods distributed along 5kpc in Galactic radius and azimuth. We decompose their distribution of stars in the V_R_-V_{phi}_ plane with the wavelet transformation and asses the statistical significance of the structures found. We detect distinct kinematic substructures (arches and more rounded groups) that diminish their azimuthal velocity as a function of Galactic radius in a continuous way, connecting volumes up to 3kpc apart in some cases. The average rate of decrease is ~23km/s/kpc. In azimuth, the variations are much smaller. We also observe different behaviours: some approximately conserve their vertical angular momentum with radius (e.g. Hercules), while others seem to have nearly constant kinetic energy (e.g. Sirius). These two trends are consistent with the approximate predictions of resonances and phase mixing, respectively. Besides, the overall spatial evolution of Hercules is consistent with being related to the outer Lindblad resonance of the Galactic bar. In addition, we detect new kinematic structures that only appear at either inner or outer Galactic radius, different from the solar neighbourhood. The strong and distinct variation observed for each kinematic substructure with position in the Galaxy, along with the characterisation of extrasolar moving groups, will allow to better model the dynamical processes affecting the velocity distributions.
368. Milky Way global survey of star clusters
ID:
ivo://CDS.VizieR/J/A+A/543/A156
Title:
Milky Way global survey of star clusters
Short Name:
J/A+A/543/A156
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a list of 650 Milky Way Stellar Clusters (MWSC) in the second quadrant of the Galaxy, found in the 2MAst (2MASS with Astrometry) catalogue. The target list was compiled on the basis of present-day lists of open, globular and candidate clusters. For confirmed clusters we determined a homogeneous set of astrophysical parameters such as membership, angular radii of the main morphological parts, proper motion, sometimes radial velocities, distance, reddening, age, tidal parameters.
369. Milky Way global survey of star clusters. II.
ID:
ivo://CDS.VizieR/J/A+A/558/A53
Title:
Milky Way global survey of star clusters. II.
Short Name:
J/A+A/558/A53
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a list of 3006 Milky Way Stellar Clusters (MWSC), found in the 2MAst (2MASS with Astrometry) catalogue. The target list was compiled on the basis of present-day lists of open, globular and candidate clusters. For confirmed clusters we determined a homogeneous set of astrophysical parameters such as membership, angular radii of the main morphological parts, mean cluster proper motions, distances, reddenings, ages, tidal parameters, and sometimes radial velocities.
370. Milky Way global survey of star clusters. III.
ID:
ivo://CDS.VizieR/J/A+A/568/A51
Title:
Milky Way global survey of star clusters. III.
Short Name:
J/A+A/568/A51
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a list of 139 new open clusters at high Galactic latitudes (|b|>18.5{deg}) that are found in the frame of the project Milky Way Star Clusters (MWSC). The target list was compiled as density enhancements using the 2MASS catalogue. For confirmed clusters we determined a homogeneous set of astrophysical parameters such as membership, angular radii of the main morphological parts, proper motion, distance, reddening, age, tidal parameters.