Initial data release from the INT Photometric H Survey of the Northern Galactic Plane (IPHAS)

Aims. We test the performance of the semi-analytic self-consistent Just-Jahreiß disc model (JJ model) with the astrometric data from the Tycho-Gaia Astrometric Solution (TGAS) sub-catalogue of the first Gaia data release (Gaia DR1), as well as the radial velocities from the fifth data release of the Radial Velocity Experiment survey (RAVE DR5). Methods. We used a sample of 19 746 thin-disc stars from the TGAS×RAVE cross-match selected in a local solar cylinder of 300 pc radius and 1 kpc height below the Galactic plane. Based on the JJ model, we simulated this sample via the forward modelling technique. First, we converted the predicted vertical density laws of the thin-disc populations into a mock sample. For this we used the Modules and Experiments in Stellar Astrophysics (MESA) Isochrones and Stellar Tracks (MIST), a star formation rate (SFR) that decreased after a peak at 10 Gyr ago, and a three-slope broken power-law initial mass function (IMF). Then the obtained mock populations were reddened with a 3D dust map and were subjected to the selection criteria corresponding to the RAVE and TGAS observational limitations as well as to additional cuts applied to the data sample. We calculated the quantities of interest separately at different heights above the Galactic plane, taking the distance error effects in horizontal and vertical directions into account separately. Results. The simulated vertical number density profile agrees well with the data. An underestimation of the stellar numbers begins at ∼800 pc from the Galactic plane, which is expected as the possible influence of populations from |z| > 1 kpc is ignored during the modelling. The lower main sequence (LMS) is found to be thinner and under-populated by 3.6% relative to the observations. The corresponding deficits for the upper main sequence (UMS) and red giant branch (RGB) are 6% and 34.7%, respectively. However, the intrinsic uncertainty related to the choice of stellar isochrones is ∼10% in the total stellar number. The vertical velocity distribution function f(|W|) simulated for the whole cylinder agrees to within 1σ with the data. This marginal agreement arises because the dynamically cold populations at heights < 200 pc from the Galactic plane are underestimated. We also find that the model gives a fully realistic representation of the vertical gradient in stellar populations when studying the Hess diagrams for different horizontal slices. We also checked and confirm the consistency of our results with the newly available second Gaia data release (DR2). Conclusions. Based on these results and considering the uncertainties in the data selection as well as the sensitivity of the simulations to the sample selection function, we conclude that the fiducial JJ model confidently reproduces the vertical trends in the thin-disc stellar population properties. Thus, it can serve as a starting point for the future extension of the JJ model to other Galactocentric distances.

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AMI Galactic Plane Survey at 16 GHz – II. Full data release with extended coverage and improved processing

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stv1728 ◽

2015 ◽

Vol 453 (2) ◽

pp. 1396-1403 ◽

Cited By ~ 4

Author(s):

Yvette C. Perrott ◽

Anna M. M. Scaife ◽

David A. Green ◽

Keith J. B. Grainge ◽

Natasha Hurley-Walker ◽

...

Keyword(s):

Galactic Plane ◽

Full Data ◽

Data Release

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THE GALACTIC PLANE INFRARED POLARIZATION SURVEY (GPIPS): DATA RELEASE 1

The Astrophysical Journal Supplement Series ◽

10.1088/0067-0049/200/2/21 ◽

2012 ◽

Vol 200 (2) ◽

pp. 21 ◽

Cited By ~ 21

Author(s):

Dan P. Clemens ◽

M. D. Pavel ◽

L. R. Cashman

Keyword(s):

Galactic Plane ◽

Data Release

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The Mopra Southern Galactic Plane CO Survey — Data Release 1

Publications of the Astronomical Society of Australia ◽

10.1017/pasa.2015.20 ◽

2015 ◽

Vol 32 ◽

Cited By ~ 20

Author(s):

Catherine Braiding ◽

M. G. Burton ◽

R. Blackwell ◽

C. Glück ◽

J. Hawkes ◽

...

Keyword(s):

Survey Data ◽

Spatial Resolution ◽

Spectral Resolution ◽

Molecular Clouds ◽

Galactic Plane ◽

Data Archive ◽

Data Release ◽

Noise Statistics ◽

Galactic Longitude

AbstractWe present observations of the first 10° of longitude in the Mopra CO survey of the southern Galactic plane, covering Galactic longitude l = 320–330° and latitude b = ±0.5°, and l = 327–330°, b = +0.5–1.0°. These data have been taken at 35-arcsec spatial resolution and 0.1 km s−1 spectral resolution, providing an unprecedented view of the molecular clouds and gas of the southern Galactic plane in the 109–115 GHz J = 1–0 transitions of 12CO, 13CO, C18O, and C17O. Together with information about the noise statistics from the Mopra telescope, these data can be retrieved from the Mopra CO website and the CSIRO-ATNF data archive.

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Initial data release and announcement of the Fish10K: Fish 10,000 Genomes Project

10.1101/787028 ◽

2019 ◽

Author(s):

Guanngyi Fan ◽

Yue Song ◽

Xiaoyun Huang ◽

Liandong Yang ◽

Suyu Zhang ◽

...

Keyword(s):

Initial Data ◽

Fish Species ◽

Technology Development ◽

Human Society ◽

Sustainable Utilization ◽

Collaborative Project ◽

Vertebrate Group ◽

Data Release ◽

International Collaborative ◽

And Storage

AbstractWith more than 30,000 species, fish are the largest and most ancient vertebrate group. Despite their critical roles in many ecosystems and human society, fish genomics lags behind work on birds and mammals. This severely limits our understanding of evolution and hinders progress on the conservation and sustainable utilization of fish. Here, we announce the Fish10K project, an international collaborative project or initiative? aiming to sequence 10,000 representative fish genomes under a systematic context within ten years, and officially welcome collaborators to join this effort. As a step towards this goal, we herein describe a feasible workflow for the procurement and storage of biospecimens, and sequencing and assembly strategies. To illustrate, we present the genomes of ten fish species from a cohort of 93 species chosen for technology development.

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The Galactic Plane Infrared Polarization Survey (GPIPS): Data Release 4

The Astrophysical Journal Supplement Series ◽

10.3847/1538-4365/ab9f30 ◽

2020 ◽

Vol 249 (2) ◽

pp. 23

Author(s):

Dan P. Clemens ◽

L. R. Cashman ◽

C. Cerny ◽

A. M. El-Batal ◽

K. E. Jameson ◽

...

Keyword(s):

Galactic Plane ◽

Data Release

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Abstract LB-102: Landscape analysis of the initial data release from AACR Project GENIE

10.1158/1538-7445.am2017-lb-102 ◽

2017 ◽

Cited By ~ 1

Author(s):

Ethan Cerami ◽

Alexander S. Baras ◽

Justin Guinney ◽

Eva Lepisto ◽

Trevor J. Pugh ◽

...

Keyword(s):

Initial Data ◽

Landscape Analysis ◽

Data Release

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The SEDIGISM survey: First Data Release and overview of the Galactic structure

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2369 ◽

2020 ◽

Vol 500 (3) ◽

pp. 3064-3082 ◽

Cited By ~ 2

Author(s):

F Schuller ◽

J S Urquhart ◽

T Csengeri ◽

D Colombo ◽

A Duarte-Cabral ◽

...

Keyword(s):

Interstellar Medium ◽

Large Scale ◽

Galactic Plane ◽

Structural Features ◽

Galactic Centre ◽

Molecular Gas ◽

Spiral Arms ◽

Star Forming ◽

Wide Range ◽

Data Release

ABSTRACT The SEDIGISM (Structure, Excitation and Dynamics of the Inner Galactic Interstellar Medium) survey used the APEX telescope to map 84 deg2 of the Galactic plane between ℓ = −60° and +31° in several molecular transitions, including 13CO (2 – 1) and C18O (2 – 1), thus probing the moderately dense (∼103 cm−3) component of the interstellar medium. With an angular resolution of 30 arcsec and a typical 1σ sensitivity of 0.8–1.0 K at 0.25 km s−1 velocity resolution, it gives access to a wide range of structures, from individual star-forming clumps to giant molecular clouds and complexes. The coverage includes a good fraction of the first and fourth Galactic quadrants, allowing us to constrain the large-scale distribution of cold molecular gas in the inner Galaxy. In this paper, we provide an updated overview of the full survey and the data reduction procedures used. We also assess the quality of these data and describe the data products that are being made publicly available as part of this First Data Release (DR1). We present integrated maps and position–velocity maps of the molecular gas and use these to investigate the correlation between the molecular gas and the large-scale structural features of the Milky Way such as the spiral arms, Galactic bar and Galactic Centre. We find that approximately 60 per cent of the molecular gas is associated with the spiral arms and these appear as strong intensity peaks in the derived Galactocentric distribution. We also find strong peaks in intensity at specific longitudes that correspond to the Galactic Centre and well-known star-forming complexes, revealing that the 13CO emission is concentrated in a small number of complexes rather than evenly distributed along spiral arms.

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The kinematics of white dwarfs from the SDSS DR12

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317006998 ◽

2017 ◽

Vol 13 (S334) ◽

pp. 294-295

Author(s):

E. García–Berro ◽

G. Skorobogatov ◽

S. Torres ◽

B. Anguiano ◽

A. Rebassa-Mansergas

Keyword(s):

White Dwarfs ◽

Galactic Plane ◽

Galactic Disk ◽

Three Dimensional ◽

Radial Distance ◽

Sloan Digital Sky Survey ◽

Original Sample ◽

Proper Motions ◽

Sky Survey ◽

Data Release

AbstractWe use the Sloan Digital Sky Survey Data Release 12, which is the largest available white dwarf catalogue to date, to study the evolution of the kinematical properties of the population of white dwarfs of the Galactic disk. We derive masses, ages, photometric distances and radial velocities for all white dwarfs with hydrogen-rich atmospheres. For those stars for which proper motions from the USNO-B1 catalogue are available, the three-dimensional components of the velocity are obtained. This subset of the original sample comprises 20,247 stars, making it the largest sample of white dwarfs with measured three-dimensional velocities. The volume probed by our sample is large, allowing us to obtain relevant kinematical information. In particular, our sample extends from a Galactocentric radial distance RG = 7.8 to 9.3 kpc, and vertical distances from the Galactic plane ranging from Z = +0.5 to –0.5 kpc.

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Gaia kinematics reveal a complex lopsided and twisted Galactic disc warp

Astronomy and Astrophysics ◽

10.1051/0004-6361/201834908 ◽

2019 ◽

Vol 627 ◽

pp. A150 ◽

Cited By ~ 14

Author(s):

M. Romero-Gómez ◽

C. Mateu ◽

L. Aguilar ◽

F. Figueras ◽

A. Castro-Ginard

Keyword(s):

Spatial Data ◽

Large Scale ◽

Galactic Plane ◽

Proper Motions ◽

Galactocentric Distance ◽

Bending Mode ◽

Data Release ◽

Kinematic Models ◽

Red Giant ◽

Galactic Warp

Context. There are few warp kinematic models of the Galaxy able to characterise both structure and kinematics, since these require high accuracy at large distances. These models are necessary to shed light on the lopsidedness of the warp and the twisting of the line-of-nodes of the stellar warp already seen in gas and dust. Aims. We use the vertical information coming from the Gaia Data Release 2 astrometric data up to G = 20 mag to characterise the structure of the Galactic warp, the related vertical motions, and the dependency of Galactic warp on age. Methods. We analyse two populations up to Galactocentric distances of 16 kpc: a young bright sample mainly formed by OB stars and an older one of red giant branch (RGB) stars. We use two methods (the pole count maps of great circle bands and Galactic longitude – proper motion in latitude lines) based on the Gaia observables, together with 2D projections of the positions and proper motions in the Galactic plane. Results. This work confirms the age dependency of the Galactic warp, both in position and kinematics, the height of the Galactic warp being of the order of 0.2 kpc for the OB sample and 1.0 kpc for the RGB at a Galactocentric distance of 14 kpc. Both methods find that the onset radius of the warp is 12 ∼ 13 kpc for the OB sample and 10 ∼ 11 kpc for the RGB. From the RGB sample, we find from Galactocentric distances larger than 10 kpc that the line-of-nodes twists away from the Sun-anticentre line towards Galactic azimuths ≈180−200° increasing with radius, though possibly influenced by extinction. Also, the RGB sample reveals a slightly lopsided stellar warp with ≈250 pc difference between the up and down sides. The line of maximum of proper motions in latitude is systematically offset from the line-of-nodes estimated from the spatial data, which our warp models predict as a kinematic signature of lopsidedness. We also show a prominent wave-like pattern of a bending mode different in the OB and RGB samples. Both positions and kinematics also reveal substructures that might not be related to the large-scale Galactic warp or to the bending mode. Conclusions. Gaia Data Release 2 data reveals a high degree of complexity in terms of both position and velocity that triggers the need for complex kinematic models flexible enough to combine both wave-like patterns and an S-shaped lopsided warp.

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