- ID:
- ivo://CDS.VizieR/J/A+A/598/A32
- Title:
- 2D decomposition of CALIFA galaxies
- Short Name:
- J/A+A/598/A32
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area Data Release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log(M*/M_{sun}_)>11), the galaxy population is dominated by galaxies modelled with a single Sersic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T>0.2. At intermediate masses (9.5<log(M*/M_{sun}_)<11), galaxies described with bulge+disc but B/T<0.2 are preponderant, whereas, at the low mass end (log(M*/M_{\sun}_)<9.5), the prevailing population is constituted by galaxies modelled with either pure discs or nuclear point sources+discs (i.e., no discernible bulge). The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62%, 28%, and 10% for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.
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- ID:
- ivo://CDS.VizieR/J/A+A/617/A64
- Title:
- 3D density & temp. profiles of 5 clusters
- Short Name:
- J/A+A/617/A64
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a detailed study of the integrated total hydrostatic mass profiles of the five most massive (M_500_^SZ^>5x10^14^M_{sun}_) galaxy 500 clusters selected at z~1 via the Sunyaev-Zel'dovich effect. These objects represent an ideal laboratory to test structure formation models where the primary driver is gravity. Optimally exploiting spatially-resolved spectroscopic information from XMM-Newton and Chandra observations, we used both parametric (forward, backward) and non-parametric methods to recover the mass profiles, finding that the results are extremely robust when density and temperature measurements are both available. Our X-ray masses at R_500_ are higher than the weak lensing masses obtained from the Hubble Space Telescope (HST), with a mean ratio of 1.39^+0.47^_-0.35_. This offset goes in the opposite direction to that expected in a scenario where the hydrostatic method yields a biased, underestimated, mass. We investigated halo shape parameters such as sparsity and concentration, and compared to local X-ray selected clusters, finding hints for evolution in the central regions (or for selection effects). The total baryonic content is in agreement with the cosmic value at R_500_. Comparison with numerical simulations shows that the mass distribution and concentration are in line with expectations. These results illustrate the power of X-ray observations to probe the statistical properties of the gas and total mass profiles in this high-mass, high-redshift regime.
- ID:
- ivo://CDS.VizieR/J/A+A/594/A85
- Title:
- 2D disk models from CO isotopologues line
- Short Name:
- J/A+A/594/A85
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Despite intensive studies of protoplanetary disks, there is still no reliable way to determine their total (gast+dust) mass and their surface density distribution, quantities that are crucial for describing both the structure and the evolution of disks up to the formation of planets. The goal of this work is to use less abundant CO isotopologues, such as ^13^CO, C^18^O and C^17^O, whose detection is routine for ALMA, to infer the gas mass of disks. Isotope-selective ects need to be taken into account in the analysis, because they can significantly modify CO isotopologues line intensities. CO isotope-selective photodissociation has been implemented in the physical-chemical code DALI (Dust And LInes) and more than 800 disk models have been run for a range of disk and stellar parameters. Dust and gas temperature structures have been computed self-consistently, together with a chemical calculation of the main atomic and molecular species. Both disk structure and stellar parameters have been investigated by varying the parameters in the grid of models. Total fluxes have been ray-traced for different CO isotopologues and for various low J- transitions for different inclinations.
4204. DD Mon BV light curves
- ID:
- ivo://CDS.VizieR/J/A+AS/125/475
- Title:
- DD Mon BV light curves
- Short Name:
- J/A+AS/125/475
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- New BV light curves of the short-period eclipsing binary system DD Mon have been obtained. Light-curve variability is seen in both B and V bands as compared with the light curves obtained in 1986 by Yamasaki et al. (1990AJ.....99.1218Y). The light curves are analyzed by using Wilson-Devinney's synthetic light-curve program, and the present photometric solution reveals that DD Mon is a near-contact binary with the secondary component filling the Roche lobe. Combined with Yamasaki et al.'s (1990AJ.....99.1218Y) spectroscopic results, absolute quantities of DD Mon are derived: mass of the primary M_1_=1.05+/-0.08M_{sun}_, mass of the secondary M_2_=0.47+/-0.04M_{sun}_, radius of the primary R_1_=1.36+/-0.04R_{sun}_, radius of the secondary R_2_=1.03+/-0.03R_{sun}_. These results show that the components of DD Mon have evolved away from the ZAMS and through a mass-transfer process to the present semi-detached state. The variation in shape of the light curve may be caused by the evolution of the system and the activity of dark spots.
- ID:
- ivo://CDS.VizieR/II/164
- Title:
- DDO Photoelectric Photometric Catalog
- Short Name:
- II/164
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalogue collects the DDO photometric data published in the astronomical literature until the end of 1988, and contains 8034 DDO measurements, concerning 6139 stars. The DDO 6-filter has the following peak wavelengths and widths: ------------------------ Filter Peak Width [nm] [nm] ------------------------ 35 346.0 38.3 38 381.5 33.0 41 416.6 8.3 42 425.7 7.3 45 451.7 7.6 48 488.6 18.6 51 (*) 513.0 13.4 ------------------------ (*) additional to DDO.
- ID:
- ivo://CDS.VizieR/V/33
- Title:
- DDO Photometry and Radial Velocities at Galactic Poles
- Short Name:
- V/33
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalogue includes the DDO photometry and the radial velocities observed for the study of the kinematics and abundance gradients of G and K stars in the Galactic poles regions.
- ID:
- ivo://CDS.VizieR/J/other/SAAOC/15.30
- Title:
- DDO photometry of E-region stars
- Short Name:
- J/other/SAAOC/15
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper describes the observations and gives the results of a series of observations of bright E-region stars (Cousins A.W.J. and Stoy R.H., 1962RGOB...49....3C) for use as zero point stars for DDO photometry in the southern hemisphere. The list comprises 45 stars, all brighter than V=6.0, and gives the colours in the instrumental system with internal s.e. +/-0.001mag and m_48_ with s.e. +/-0.002mag. The observed m_48_ is indistinguishable from McClure's system and has the same zero point (+/-0.002mag). The individual E-region zero points have been established with s.e. +/-0.001 relative to the instrumental system, but the colour equations (and zero point corrections) to transform the instrumental colours to McClure's system have still to be finalised. For a description of the DDO photometric system, see e.g. <GCPD/12>
- ID:
- ivo://CDS.VizieR/J/A+A/566/A120
- Title:
- 3D dust extinction in Milky Way bulge
- Short Name:
- J/A+A/566/A120
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Three dimensional interstellar extinction maps provide a powerful tool for stellar population analysis. However, until now, these 3D maps were rather limited by sensitivity and spatial resolution. We use data from the VISTA Variables in the Via Lactea survey together with the Besancon stellar population synthesis model of the Galaxy to determine interstellar extinction as a function of distance in the Galactic bulge covering -10<l<10 and -10<b<5. We adopted a recently developed method to calculate the colour excess. First we constructed the H-Ks vs. Ks and J-Ks vs. Ks colour-magnitude diagrams based on the VVV catalogues that matched 2MASS. Then, based on the temperature-colour relation for M giants and the distance-colour relations, we derived the extinction as a function of distance. The observed colours were shifted to match the intrinsic colours in the Besancon model as a function of distance iteratively. This created an extinction map with three dimensions: two spatial and one distance dimension along each line of sight towards the bulge. We present a 3D extinction map that covers the whole VVV area with a resolution of 6'x6', for J-Ks and H-Ks using distance bins of 0.5-1.0kpc. The high resolution and depth of the photometry allows us to derive extinction maps for a range of distances up to 10kpc and up to 30 magnitudes of extinction in AV (3.0mag in AKs). Integrated maps show the same dust features and consistent values as other 2D maps. We discuss the spatial distribution of dust features in the line of sight, which suggests that there is much material in front of the Galactic bar, specifically between 5-7kpc. We compare our dust extinction map with the high-resolution ^12^CO maps (NANTEN2) towards the Galactic bulge, where we find a good correlation between ^12^CO and A_V_. We determine the X factor by combining the CO map and our dust extinction map. Our derived average value X=2.5+/-0.47x10^20^/(cm^2^.K.km/s) is consistent with the canonical value of the Milky Way. The X-factor decreases with increasing extinction.
- ID:
- ivo://CDS.VizieR/II/68
- Title:
- Dearborn Catalogue of faint red stars
- Short Name:
- II/68
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Dearborn Survey is the result of a survey of faint red stars conducted at the Dearborn Observatory from about 1932 to 1947. It covers the declination range -4.5deg to +90deg (54% of the Sky), and consisted of over 1800 direct plates and spectrograms carrying single or multiple exposures varying from a second to 4 hours. The magnitudes in the catalog were obtained from direct plates mostly sensitive in the 0.55-0.64{mu}m wavelength region. The spectral types were obtained from objective-prism plates with red-sensitive emulsion, and were classified on the visibility of the TiO bands.
- ID:
- ivo://CDS.VizieR/J/A+A/653/A53
- Title:
- DEATHSTAR. II. The S-type
- Short Name:
- J/A+A/653/A53
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- We present the re-calibrated and re-imaged fits-cubes of the second set of data from the DEATHSTAR project (DEtermining Accurate mass-loss rates for THermally pulsing AGB STARs, www.astro.uu.se/deathstar): the S-type stars. Fifteen S-type southern AGB stars were mapped in Bands 6 and 7 with the Atacama Compact Array (ACA). The generated beams have sizes of 4-8 and 3-6-arcseconds in Band 6 and 7, respectively. The rms noise level reached is typically 50-70 and 100-150mJy/beam in Band 6 and 7, respectively. The beam sizes and rms values for each source are listed in the paper together with the description of the reduction process, the analysis of the cubes and tentative line detections.