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- ID:
- ivo://jao.alma/tap_na
- Title:
- Official ALMA Table Access (NA server at NRAO)
- Short Name:
- ALMA TAP NA
- Date:
- 03 Jun 2022 10:00:06
- Publisher:
- Joint ALMA Observatory (JAO)
- Description:
- The official ALMA TAP service. It provides an extended ObsCore 1.1 view of all ALMA observations.
- ID:
- ivo://CDS.VizieR/J/MNRAS/436/953
- Title:
- OGLE-LMC-CEP-0227 RV and VI[3.6] curves
- Short Name:
- J/MNRAS/436/953
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A novel method of analysis of double-lined eclipsing binaries containing a radially pulsating star is presented. The combined pulsating-eclipsing light curve is built up from a purely eclipsing light-curve grid created using an existing modelling tool. For every pulsation phase, the instantaneous radius and surface brightness are taken into account, being calculated from the disentangled radial velocity curve of the pulsating star and from its out-of-eclipse pulsational light curve and the light ratio of the components, respectively. The best model is found using the Markov chain Monte Carlo method. The method is applied to the eclipsing binary Cepheid OGLE-LMC-CEP-0227 (P_puls_=3.80d, P_orb_=309d). We analyse a set of new spectroscopic and photometric observations for this binary, simultaneously fitting OGLE V-band, I-band and Spitzer 3.6{mu}m photometry. We derive a set of fundamental parameters of the system significantly improving the precision comparing to the previous results obtained by our group. The Cepheid mass and radius are M_1_=4.165+/-0.032M_{sun}_ and R_1_=34.92+/-0.34R{sun}, respectively. For the first time a direct, geometrical and distance-independent determination of the Cepheid projection factor is presented. The value p=1.21+/-0.03(stat.)+/-0.04(syst.) is consistent with theoretical expectations for a short-period Cepheid and interferometric measurements for {delta} Cep. We also find a very high value of the optical limb darkening coefficients for the Cepheid component, in strong disagreement with theoretical predictions for static atmospheres at a given surface temperature and gravity.
- ID:
- ivo://CDS.VizieR/J/A+A/610/A74
- Title:
- OJ 287 far-infrared photometry
- Short Name:
- J/A+A/610/A74
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The blazar OJ 287 has shown a ~~12 year quasi-periodicity over more than a century, in addition to the common properties of violent variability in all frequency ranges. It is the strongest known candidate to have a binary singularity in its central engine. We aim to better understand the different emission components by searching for correlated variability in the flux over four decades of frequency measurements. We combined data at frequencies from the millimetric to the visible to characterise the multifrequency light curve in April and May 2010. This includes the only photometric observations of OJ 287 made with the Herschel Space Observatory: five epochs of data obtained over 33 days at 250, 350, and 500um with Herschel-SPIRE. Although we find that the variability at 37GHz on timescales of a few weeks correlates with the visible to near-IR spectral energy distribution (SED), there is a small degree of reddening in the continuum at lower flux levels that is revealed by the decreasing rate of decline in the light curve at lower frequencies. However, we see no clear evidence that a rapid flare detected in the light curve during our monitoring in the visible to near-IR light curve is seen either in the Herschel data or at 37GHz, suggesting a low-frequency cut-off in the spectrum of such flares. We see only marginal evidence of variability in the observations with Herschel over a month, although this may be principally due to the poor sampling. The spectral energy distribution between 37 GHz and the visible can be characterised by two components of approximately constant spectral index: a visible to far-IR component of spectral index {alpha}=-0.95, and a far-IR to millimetric spectral index of {alpha}=0.43. There is no evidence of an excess of emission that would be consistent with the 60um dust bump found in many active galactic nuclei.
- ID:
- ivo://CDS.VizieR/J/MNRAS/482/698
- Title:
- Ophiuchus DIsc Survey Employing ALMA (ODISEA). I.
- Short Name:
- J/MNRAS/482/698
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We introduce the Ophiuchus DIsc Survey Employing ALMA (ODISEA), a project aiming to study the entire population of Spitzer-selected protoplanetary discs in the Ophiuchus Molecular Cloud (~300 objects) from both millimetre continuum and CO isotopologues data. Here we present 1.3mm/230GHz continuum images of 147 targets at 0.2" (28au) resolution and a typical rms of 0.15mJy. We detect a total of 133 discs, including the individual components of 11 binary systems and 1 triple system. 60 of these discs are spatially resolved. We find clear substructures (inner cavities, rings, gaps, and/or spiral arms) in eight of the sources and hints of such structures in another four discs. We construct the disc luminosity function for our targets and perform preliminary comparisons to other regions. A simple conversion between flux and dust mass (adopting standard assumptions) indicates that all discs detected at 1.3mm are massive enough to form one or more rocky planets. In contrast, only ~50 discs (~1/3 of the sample) have enough mass in the form of dust to form the canonical 10M_{Earth}_ core needed to trigger runaway gas accretion and the formation of gas giant planets, although the total mass of solids already incorporated into bodies larger than cm scales is mostly unconstrained. The distribution in continuum disc sizes in our sample is heavily weighted towards compact discs: most detected discs have radii <15au, while only 23 discs (~15% of the targets) have radii >30au.
- ID:
- ivo://CDS.VizieR/J/A+A/586/A139
- Title:
- Optical ident. and redshifts of Planck SZ sources
- Short Name:
- J/A+A/586/A139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of approximately three years of observations of Planck Sunyaev-Zeldovich (SZ) sources with telescopes at the Canary Islands observatories as part of the general optical follow-up programme undertaken by the Planck Collaboration. In total, 78 SZ sources are discussed. Deep-imaging observations were obtained for most of these sources; spectroscopic observations in either in long-slit or multi-object modes were obtained for many. We effectively used 37.5 clear nights. We found optical counterparts for 73 of the 78 candidates. This sample includes 53 spectroscopic redshift determinations, 20 of them obtained with a multi-object spectroscopic mode. The sample contains new redshifts for 27 Planck clusters that were not included in the first Planck SZ source catalogue (PSZ1).
- ID:
- ivo://CDS.VizieR/J/A+A/530/A90
- Title:
- Optically bright post-AGB population of LMC
- Short Name:
- J/A+A/530/A90
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We construct a catalogue of the optically bright post-AGB stars in the LMC. The sample forms an ideal testbed for stellar evolution theory predictions of the final phase of low- and intermediate-mass stars, because the distance and hence luminosity and also the current and initial mass of these objects is well constrained.
- ID:
- ivo://CDS.VizieR/J/ApJ/671/1784
- Title:
- Ori OB1 IRAC/MIPS observations
- Short Name:
- J/ApJ/671/1784
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new Spitzer observations of two fields in the Orion OB1 association. We report IRAC/MIPS observations for 115 confirmed members and 41 photometric candidates of the ~10Myr 25 Orionis aggregate in the OB1a subassociation, and 106 confirmed members and 65 photometric candidates of the 5Myr region located in the OB1b subassociation.
- ID:
- ivo://CDS.VizieR/J/ApJS/217/7
- Title:
- Orion A dense cores based on 1.1mm and C^18^O
- Short Name:
- J/ApJS/217/7
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present Orion A giant molecular cloud core catalogs, which are based on a 1.1mm map with an angular resolution of 36" (~0.07pc) and C^18^O (J=1-0) data with an angular resolution of 26.4" (~0.05pc). We have cataloged 619 dust cores in the 1.1mm map using the Clumpfind method. The ranges of the radius, mass, and density of these cores are estimated to be 0.01-0.20pc, 0.6-1.2x10^2^M_{sun}_ , and 0.3x10^4^-9.2x10^6^cm^-3^, respectively. We have identified 235 cores from the C^18^O data. The ranges of the radius, velocity width, LTE mass, and density are 0.13-0.34pc, 0.31-1.31km/s, 1.0-61.8M_{sun}_ , and (0.8-17.5)x10^3^cm^-3^, respectively. From the comparison of the spatial distributions between the dust and C^18^O cores, four types of spatial relations were revealed: (1) the peak positions of the dust and C^18^O cores agree with each other (32.4% of the C^18^O cores), (2) two or more C^18^O cores are distributed around the peak position of one dust core (10.8% of the C^18^O cores), (3) 56.8% of the C^18^O cores are not associated with any dust cores, and (4) 69.3% of the dust cores are not associated with any C^18^O cores.
- ID:
- ivo://CDS.VizieR/J/A+A/600/A141
- Title:
- Orion A integral shaped filament image
- Short Name:
- J/A+A/600/A141
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the fragmentation of the nearest high line-mass filament, the integral shaped filament (ISF, line-mass ~400M_{sun}_/pc) in the Orion A molecular cloud. We have observed a 1.6pc long section of the ISF with the Atacama Large Millimetre/submillimeter Array (ALMA) at 3mm continuum emission, at a resolution of ~3" (1200AU). We identify from the region 43 dense cores with masses about a solar mass. 60% of the ALMA cores are protostellar and 40% are starless. The nearest neighbour separations of the cores do not show a preferred fragmentation scale; the frequency of short separations increases down to 1200AU. We apply a two-point correlation analysis on the dense core separations and show that the ALMA cores are significantly grouped at separations below ~17000AU and strongly grouped below ~6000AU. The protostellar and starless cores are grouped differently: only the starless cores group strongly below ~6000AU. In addition, the spatial distribution of the cores indicates periodic grouping of the cores into groups of ~30000AU in size, separated by ~50000AU. The groups coincide with dust column density peaks detected by Herschel. These results show hierarchical, two-mode fragmentation in which the maternal filament periodically fragments into groups of dense cores. Critically, our results indicate that the fragmentation models for lower line-mass filaments (~16M_{sun}_/pc) fail to capture the observed properties of the ISF. We also find that the protostars identified with Spitzer and Herschel in the ISF are grouped at separations below ~17000AU. In contrast, young stars with disks do not show significant grouping. This suggests that the grouping of dense cores is partially retained over the protostar lifetime, but not over the lifetime of stars with disks. This is in agreement with a scenario where protostars are ejected from the maternal filament by the slingshot mechanism, a model recently proposed for the ISF. The separation distributions of the dense cores and protostars may also provide an evolutionary tracer of filament fragmentation.
