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3621. Deep NIR catalogue of HIZOA galaxies
ID:
ivo://CDS.VizieR/J/MNRAS/462/3386
Title:
Deep NIR catalogue of HIZOA galaxies
Short Name:
J/MNRAS/462/3386
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a deep near-infrared (NIR; J, H, and K_s_ bands) photometric catalogue of sources from the Parkes HI Zone of Avoidance (HIZOA) survey, which forms the basis for an investigation of the matter distribution in the Zone of Avoidance. Observations were conducted between 2006 and 2013 using the Infrared Survey Facility (IRSF), a 1.4-m telescope situated at the South African Astronomical Observatory site in Sutherland. The images cover all 1108 HIZOA detections and yield 915 galaxies. An additional 105 bright 2MASS galaxies in the southern ZOA were imaged with the IRSF, resulting in 129 galaxies. The average K_s_-band seeing and sky background for the survey are 1.38-arcsec and 20.1mag, respectively. The detection rate as a function of stellar density and dust extinction is found to depend mainly on the HI mass of the HI detected galaxies, which in principal correlates with the NIR brightness of the spiral galaxies. The measured isophotal magnitudes are of sufficient accuracy (errors ~0.02mag) to be used in a Tully-Fisher analysis. In the final NIR catalogue, 285 galaxies have both IRSF and 2MASS photometry (180 HIZOA plus 105 bright 2MASX galaxies). The K_s_-band isophotal magnitudes presented in this paper agree, within the uncertainties, with those reported in the 2MASX catalogue. Another 30 galaxies, from the HIZOA northern extension, are also covered by UKIDSS Galactic Plane Survey (GPS) images, which are one magnitude deeper than our IRSF images. A modified version of our photometry pipeline was used to derive the photometric parameters of these UKIDSS galaxies. Good agreement was found between the respective K_s_-band isophotal magnitudes. These comparisons confirm the robustness of the isophotal parameters and demonstrate that the IRSF images do not suffer from foreground contamination, after star removal, nor underestimate the isophotal fluxes of ZoA galaxies.
3622. Deep NIR imaging of {rho} Oph cloud core
ID:
ivo://CDS.VizieR/J/ApJ/719/550
Title:
Deep NIR imaging of {rho} Oph cloud core
Short Name:
J/ApJ/719/550
Date:
21 Oct 2021
Publisher:
CDS
Description:
A search for young substellar objects in the {rho} Oph cloud core region has been made with the aid of multiband profile-fitting point-source photometry of the deep-integration Combined Calibration Scan images of the 2MASS extended mission in the J, H, and Ks bands, and Spitzer IRAC images at 3.6, 4.5, 5.8, and 8.0um. The field of view of the combined observations was 1{deg}x9.3', and the 5{sigma} limiting magnitude at J was 20.5. Comparison of the observed spectral energy distributions with the predictions of the COND and DUSTY models, for an assumed age of 1Myr, supports the identification of many of the sources with brown dwarfs and enables the estimation of effective temperature, T_eff_. The cluster members are then readily distinguishable from background stars by their locations on a plot of flux density versus T_eff_. The range of estimated T_eff_ values extends down to ~750K which, based on the COND model, would suggest the presence of objects of sub-Jupiter mass. The results also suggest that the mass function for the {rho} Oph cloud resembles that of the {sigma} Orionis cluster based on a recent study, with both rising steadily toward lower masses. The other main result from our study is the apparent presence of a progressive blueward skew in the distribution of J-H and H-Ks colors, such that the blue end of the range becomes increasingly bluer with increasing magnitude. We suggest that this behavior might be understood in terms of the "ejected stellar embryo" hypothesis, whereby some of the lowest-mass brown dwarfs could escape to locations close to the front edge of the cloud, and thereby be seen with less extinction.
3623. Deep NIR photometry of HI galaxies in ZoA
ID:
ivo://CDS.VizieR/J/MNRAS/443/41
Title:
Deep NIR photometry of HI galaxies in ZoA
Short Name:
J/MNRAS/443/41
Date:
21 Oct 2021
Publisher:
CDS
Description:
Current studies of the peculiar velocity flow field in the local Universe are limited by either the lack of detection or accurate photometry for galaxies at low Galactic latitudes. The contribution to the dynamics of the Local Group of the largely unknown mass distribution in this 'Zone of Avoidance' (ZoA) remains controversial. We present here the results of a pilot project to obtain deep near-infrared (NIR) observations of galaxies detected in the systematic Parkes deep HI survey of the ZoA (HIZOA) - 578 galaxies with recession velocities out to 6000km/s were observed with the 1.4m InfraRed Survey Facility SIRIUS (Simultaneous InfraRed Imager for Unbiased Surveys) camera providing J, H and Ks imaging 2mag deeper than 2MASS. After star subtraction, the resulting isophotal magnitudes and inclinations of ZoA galaxies are of sufficient accuracy (magnitude errors under 0.1mag even at high extinction) to ultimately be used to determine cosmic flow fields 'in' the ZoA via the NIR Tully-Fisher relation. We further used the observed NIR colours to assess the ratio of the true extinction to the Diffuse Infrared Background Experiment/IRAS extinction deep into the dust layers of the Milky Way. The derived ratio was found to be 0.87 across the HIZOA survey region with no significant variation with Galactic latitude or longitude. This value is in excellent agreement with the completely independently derived factor of 0.86 by Schlafly & Finkbeiner (2010ApJ...725.1175S) based on Sloan data far away from the Milky Way.
3624. Deep NIR survey of the Pipe Nebula. II.
ID:
ivo://CDS.VizieR/J/ApJ/725/2232
Title:
Deep NIR survey of the Pipe Nebula. II.
Short Name:
J/ApJ/725/2232
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a new set of high-resolution dust extinction maps of the nearby and essentially starless Pipe Nebula molecular cloud. The maps were constructed from a concerted deep near-infrared imaging survey with the ESO-VLT, ESO-NTT, CAHA 3.5m telescopes, and 2MASS data. The new maps have a resolution three times higher than the previous extinction map of this cloud by Lombardi et al. (2006A&A...454..781L) and are able to resolve structures down to 2600AU. We detect 244 significant extinction peaks across the cloud. These peaks have masses between 0.1 and 18.4M_{sun}_, diameters between 1.2 and 5.7x10^4^AU (0.06 and 0.28pc), and mean densities of about 10^4^cm^-3^, all in good agreement with previous results. From the analysis of the mean surface density of companions we find a well-defined scale near 1.4x10^4^AU below which we detect a significant decrease in structure of the cloud. This scale is smaller than the Jeans length calculated from the mean density of the peaks. The surface density of peaks is not uniform but instead it displays clustering. Extinction peaks in the Pipe Nebula appear to have a spatial distribution similar to the stars in Taurus, suggesting that the spatial distribution of stars evolves directly from the primordial spatial distribution of high-density material.
3625. Deep NIR survey toward Aquila. I. MHOs
ID:
ivo://CDS.VizieR/J/ApJS/219/21
Title:
Deep NIR survey toward Aquila. I. MHOs
Short Name:
J/ApJS/219/21
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have performed an unbiased, deep near-infrared survey toward the Aquila molecular cloud with a sky coverage of ~1deg^2^. We identified 45 molecular hydrogen emission-line objects (MHOs), of which only 11 were previously known. Using the Spitzer archival data, we also identified 802 young stellar objects (YSOs) in this region. Based on the morphology and the location of MHOs and YSO candidates, we associate 43 MHOs with 40 YSO candidates. The distribution of jet length shows an exponential decrease in the number of outflows with increasing length, and the molecular hydrogen outflows seem to be oriented randomly. Moreover, there is no obvious correlation between jet lengths, jet opening angles, or jet H_2_ 1-0 S(1) luminosities and the spectral indices of the possible driving sources in this region. We also suggest that molecular hydrogen outflows in the Aquila molecular cloud are rather weak sources of turbulence, unlikely to generate the observed velocity dispersion in the region of survey.
3626. Deep Objective-Prism Survey for LMC Members
ID:
ivo://CDS.VizieR/III/113A
Title:
Deep Objective-Prism Survey for LMC Members
Short Name:
III/113A
Date:
21 Oct 2021
Publisher:
CDS
Description:
The catalog contains 1273 proven or probable Large Magellanic Cloud (LMC) members, identified on plates taken with the Curtis-Schmidt telescope at Cerro Tololo Inter-American Observatory in Chile. The stars are generally brighter than photographic magnitude 14 and are identified on charts published by Hodge and Wright (1967) and reproduced in the source publication (1970CoTol..89....1S). Approximate spectral types were determined by examination of the 580 Angstroms/mm (at H{gamma}) objective-prism spectra; approximate 1975 positions were obtained by measuring relative to the 1975 coordinate grids on the Uppsala-Mount Stromlo Atlas of the LMC (Gascoigne and Westerlund 1961), and approximate photographic magnitudes were determined by averaging image density measures from the plates and image-diameter measures on the "B" charts of Hodge and Wright (1967SAOP.4699....1H). The catalog includes an identification number (Sk), HD(E) number, Cape Photographic Durchmusterung number, right ascension and declination (equinox B1975), spectral type, photographic magnitude, and alternate identifications. The machine version, updated in September 1986, includes corrections supplied by the author in 1985; thus, it differs somewhat from the published version. Accurate positions, and cross-identifications with the modern surveys, were determined by Brian Skiff in 2008, and make up the "sk_pos.dat" file. This work is based on a file prepared through great effort by Mati Morel in 1999. Brian Skiff examined every object on DSS cut-outs to make sure the star chosen matched the Sanduleak charts. The Goddard SkyView utility was used, looking at an 0.07{deg} (4'x4') field from the DSS1 (short-V plate), DSS2 far-red, and 2MASS J-band images. These three have the shallowest effective exposure (these are bright stars!), and usually the best image quality to check for companions etc as well as star colors. Precise coordinates were then obtained via VizieR mainly from UCAC2, but occasionally elsewhere as indicated in the column 's' for each star. The list was also matched against Tycho-2 and the GSC, and the Massey et al. photometric survey from 2002ApJS..141...81M (Cat. II/236). The file "sk_pos.dat" includes also Sanduleak's original approximate spectral types, and approximative V magnitudes that Mati Morel adopted from the work of the Marseille group; some missing HD(E) and CPD names were also added. It should be noticed also that the file has 1275 entries, 3 stars being resolved into resolved pairs. The notes includes Sanduleak's original notes, as well as remarks added by Brian Skiff in the course of his verifications.
3627. Deep OB star population in Carina
ID:
ivo://CDS.VizieR/J/MNRAS/465/1807
Title:
Deep OB star population in Carina
Short Name:
J/MNRAS/465/1807
Date:
21 Oct 2021
Publisher:
CDS
Description:
Massive OB stars are critical to the ecology of galaxies, and yet our knowledge of OB stars in the Milky Way, fainter than V~12, remains patchy. Data from the VST Photometric H-alpha Survey (VPHAS+) permit the construction of the first deep catalogues of blue excess-selected OB stars, without neglecting the stellar field. A total of 14900 candidates with 2MASS cross-matches are blue-selected from a 42 square-degree region in the Galactic longitude range 282{deg}<l<293{deg} Spectral energy distribution fitting is performed on these candidates' combined VPHAS+ u/g/r/i and 2MASS J/H/K magnitudes. This delivers: effective temperature constraints, statistically separating O from early-B stars; high-quality extinction parameters, A_0_ and R_V_ (random errors typically <0.1). The high confidence O-B2 candidates number 5915 and a further 5170 fit to later B spectral type. Spectroscopy of 276 of the former confirms 97% of them. The fraction of emission line stars among all candidate B stars is 7-8%. Greyer (R_V_>3.5) extinction laws are ubiquitous in the region, over the distance range 2.5-3kpc to ~10kpc. Near prominent massive clusters, R_V_ tends to rise, with particularly large and chaotic excursions to R_V_~5 seen in the Carina Nebula. The data reveal a hitherto unnoticed association of 108 O-B2 stars around the O5If+ star LSS 2063 (l=289.77{deg}, b=-1.22{deg}). Treating the OB star scale-height as a constant within the thin disk, we find an orderly mean relation between extinction (A_0_) and distance in the Galactic longitude range, 287.6{deg}<l< 293.5{deg}, and infer the subtle onset of thin-disk warping. A halo around NGC 3603, roughly a degree in diameter, of ~500 O-B2 stars with 4<A_0_(mag)<7 is noted.
3628. Deep optical and infrared photometry of Sh2-305
ID:
ivo://CDS.VizieR/J/ApJ/891/81
Title:
Deep optical and infrared photometry of Sh2-305
Short Name:
J/ApJ/891/81
Date:
17 Jan 2022 00:38:10
Publisher:
CDS
Description:
Using our deep optical and near-infrared photometry along with multiwavelength archival data, we here present a detailed study of the Galactic HII region Sh 2-305 to understand the star/star-cluster formation. On the basis of excess infrared emission, we have identified 116 young stellar objects (YSOs) within a field of view of ~18.5'x18.5' around Sh 2-305. The average age, mass, and extinction (AV) for this sample of YSOs are 1.8Myr, 2.9M_{sun}_, and 7.1mag, respectively. The density distribution of stellar sources along with minimal spanning tree calculations on the location of YSOs reveals at least three stellar subclusterings in Sh 2-305. One cluster is seen toward the center (i.e., Mayer 3), while the other two are distributed toward the north and south directions. Two massive O-type stars (VM2 and VM4; ages ~5Myr) are located at the center of the Sh 2-305 HII region. The analysis of the infrared and radio maps traces the photon-dominant regions (PDRs) in Sh 2-305. The association of the younger generation of stars with the PDRs is also investigated in Sh2-305. This result suggests that these two massive stars might have influenced the star formation history in Sh 2-305. This argument is also supported by the calculation of various pressures driven by massive stars, the slope of the mass function/K-band luminosity function, star formation efficiency, fraction of Class I sources, and mass of the dense gas toward the subclusterings in Sh 2-305.
3629. Deep Optical Catalog of galaxy systems
ID:
ivo://CDS.VizieR/J/ApJ/518/69
Title:
Deep Optical Catalog of galaxy systems
Short Name:
J/ApJ/518/69
Date:
21 Oct 2021
Publisher:
CDS
Description:
We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, & White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}>0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).
3630. Deep optical photometry in M31
ID:
ivo://CDS.VizieR/J/ApJS/184/152
Title:
Deep optical photometry in M31
Short Name:
J/ApJS/184/152
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using the Advanced Camera for Surveys on the Hubble Space Telescope, we have obtained deep optical images reaching well below the oldest main-sequence turnoff in six fields of the Andromeda Galaxy. The fields fall at four positions on the southeast minor axis, one position in the giant stellar stream, and one position on the northeast major axis. These data were obtained as part of three large observing programs designed to probe the star formation history of the stellar population in various structures of the galaxy. In this paper, we present the images, catalogs, and artificial star tests for these observing programs as a supplement to the analyses published previously. These high-level science products are also archived at the Multimission Archive at the Space Telescope Science Institute.

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