2024-03-29T00:06:00Z
https://zenodo.org/oai2d
oai:zenodo.org:7312088
2022-11-11T19:58:10Z
openaire
user-vltihow2022
Rojas, Daniela
Calderon, Jeronimo
Piña, Daniel
Chaparro, Germán
Labdon, Aaron
2022-11-10
<p>Presentation of the reduction, calibration, and reconstruction process of images of the Young Stellar Object (YSO) MWC 275 (HD 163296) done by the co-authors as part of the practical sessions of the VLTI-HOW 2022 workshop. The processed data contains three observation runs recorded during 2019 for three different setups using the VLTI instrument PIONIER (Precision Integrated-Optics Near-Infrared Imaging ExpeRiment). The image reconstruction was done using two methods: BSMEM and SQUEEZE. A model of a possible disk was also fitted to the provided data using PMOIRED.</p>
https://doi.org/10.5281/zenodo.7312088
oai:zenodo.org:7312088
eng
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7312087
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
VLTI-HOW
Interferometric image reconstruction
Optical interferometry
PIONIER
Young Stellar Objects
Circumstellar Disks
Image reconstruction of MWC 275 using PIONIER data
info:eu-repo/semantics/lecture
oai:zenodo.org:7351297
2022-11-23T14:26:30Z
openaire
user-vltihow2022
Mella, Guillaume
Bourgès, Laurent
2022-11-23
<p>The Optical interferometry Database (OiDB) provides a convenient solution to query optical interferometry data (OIFITS format) as well as regularly-updated observation logs obtained with a wide range of interferometric instruments. It relies on Virtual Observatory standards and tools to increase diffusion and operability.</p>
https://doi.org/10.5281/zenodo.7351297
oai:zenodo.org:7351297
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7351296
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
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vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
OiDB - A global database for optical interferometry
info:eu-repo/semantics/lecture
oai:zenodo.org:7507057
2023-01-06T14:26:39Z
openaire
user-vltihow2022
Ohnaka, Keiichi
2023-01-05
<p>Introduction to astronomical interferometry--its theoretical principles and practical aspects.</p>
https://doi.org/10.5281/zenodo.7507057
oai:zenodo.org:7507057
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7507056
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
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vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
Introduction to astronomical interferometry
info:eu-repo/semantics/lecture
oai:zenodo.org:7250266
2022-10-26T02:26:22Z
openaire
user-vltihow2022
Trisha Bhowmik
2022-10-25
<p>[BHB2007]-1 is an accreting young stellar object which is surrounded by a protoplanetary disk with an enormous gap (~70 au wide). This cavity might have been carved by a very young brown dwarf candidate present at a distance of 0''.32. To date, the presence of this candidate has only been detected in the radio (VLA) and NACO's L' filter, limiting to constrain the mass accurately. </p>
<p>We have GRAVITY observing time to extract the K-band spectrum of the companion candidate for the first time. We aim to constrain the dynamical mass of the companion, characterize it with atmospheric models and perform high-precision astrometry to constrain its position. A successful observation would confirm the presence of the brown dwarf companion candidate. Additionally, we also would be able to observe the circumplanetary environment with a much higher resolution compared to the previous observations.</p>
https://doi.org/10.5281/zenodo.7250266
oai:zenodo.org:7250266
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7250211
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
protoplanetary disk
young stellar object
brown dwarf
Detecting a brown dwarf around a YSO BHB2007-1 with GRAVITY
info:eu-repo/semantics/conferencePoster
oai:zenodo.org:7296810
2022-11-07T14:49:37Z
openaire
user-vltihow2022
Novak, Mathais
Parashivamurthy, Harshitha Mysore
Bhowmik, Trisha
Rajkumar, Anitha Raj
Oliveros Gomez, Natalia
Medina, Sofia
2022-10-21
<p>This is the final presentation and a summary of the work we did during the VLTI-HOW workshop under Mathais Novak, University of Cambridge. The data from the night of September 21, 2018 of the system beta pic b obtained from the GRAVITY-VLTI instrument in the Paranal observatory was downloaded from the ESO archive and reduced manually along with the ESO pipeline gravity. We further made corrections to the reduced data and used pipelines, Clean Gravity and exoGravity for astrometry study. A spectrum was extracted of the exoplanet, beta pic b which showed the Bracket gamma peak. Later, DIRFT-PHOENIX model was used to fit the spectrum, yielding the estimated median parametric values and demonstrating a good fit. Finally, a calculated mass of 9.2 MJ, and the temperature 1.72e+03 K was obtained.</p>
https://doi.org/10.5281/zenodo.7296810
oai:zenodo.org:7296810
eng
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7296809
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
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vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
exoplanets, GRAVITY, interferometry.
GRAVITY on 𝛽 Pic b
info:eu-repo/semantics/lecture
oai:zenodo.org:7504485
2023-01-05T14:26:29Z
openaire
user-vltihow2022
Labdon, Aaron
2023-01-04
<p>The VLTI view of protoplanetary disks. A review of observations of planet forming disks around young stars with the very large telescope interferometer. Including some tips and tricks for analysing your own VLTI observations.</p>
https://doi.org/10.5281/zenodo.7504485
oai:zenodo.org:7504485
eng
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7504484
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
The VLTI view of protoplanetary disks
info:eu-repo/semantics/lecture
oai:zenodo.org:7675699
2023-02-27T12:17:06Z
openaire
user-vltihow2022
Borges Fernandes, Marcelo
2023-02-24
<p>Presentation about star formation theory, young stellar objects and the contribution from optical interferometry.</p>
https://doi.org/10.5281/zenodo.7675699
oai:zenodo.org:7675699
eng
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7675698
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
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vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
Star formation, YSO, interferometry
Star Formation and YSO Introduction
info:eu-repo/semantics/lecture
oai:zenodo.org:7244493
2022-10-27T13:10:10Z
openaire
user-vltihow2022
Lohmann, Felipe
Schnorr-Müller, Allan
Trevisan, Marina
2022-10-21
<p>The population of quiescent galaxies undergoes significant changes over time. Ten billion years ago, these objects were generally compact and had a prominent disk with significant rotational support. In the local universe, however, they are larger by a factor of 3-5 and are mostly dispersion-supported ellipsoids. Still, there exists a rare population of galaxies that are still compact in the present-day universe, whose nature is still not well understood. One possibility is that these objects are galaxies formed at high redshifts that evolved passively. Or, they could have been formed at lower redshifts, but in similar conditions as the high redshift compact galaxies. In a recent work, our group studied a sample of compact quiescent galaxies from the MaNGA survey and found that, compared to average-sized quiescent galaxies, compact galaxies have similar ages, although being more metal rich and having a higher abundance of <span class="math-tex">\(\alpha\)</span> elements. However, while compact galaxies have a quiet accretion history, the opposite is true for average-sized galaxies. Thus, it is not clear whether the differences between the two populations are related to their high redshift progenitors or to a difference in their post-quenching evolution, e.g. the occurrence of mergers. Also, the local compact galaxies were shown to be the likely descendants of post-starburst galaxies, which can play a role in the observed properties of these objects. Since it is not possible to recover a detailed star formation history from archeological studies of local compact quiescent galaxies, an alternative is to study cosmological simulations, which reproduce various observables and allow a thorough analysis of the evolution of galaxies across time. The aim of the work is to study the population of compact quiescent galaxies at <span class="math-tex">\(z=0\)</span> in the IllustrisTNG cosmological simulation and see how the evolution of these objects differ from that of the population of average-sized quiescent galaxies. We compare their kinematics, stellar populations, environmental features and star-formation histories in order to fully characterize the differences between them. These results are then compared to those of recent studies in the literature in order to propose a scenario for the evolution of compact quiescent galaxies.</p>
https://doi.org/10.5281/zenodo.7244493
oai:zenodo.org:7244493
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7244492
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
The formation and evolution of massive compact galaxies in cosmological simulations
info:eu-repo/semantics/conferencePoster
oai:zenodo.org:7255841
2022-10-27T13:10:11Z
openaire
user-vltihow2022
Ortiz-Leon, Gisela
2022-10-27
<p>High precision astrometry at the ≈10 uas level is now routinely achieved from the ground with the Very Long BaseIine Interferometry (VLBI) technique. The milli-arcsecond (mas) angular resolution of VLBI instruments allows to resolve binary systems were angular separations can be as small as a few mas. In addition, high precision astrometry allows searching for unseen companions, by the detection of the astrometric signature or “wobble” due to the gravitational pull of the companion. We have used astrometry at radio wavelengths to search for giant planets around very low mass stars, which are difficult to find by other techniques. In this contribution, we present the properties of low-mass young binaries and of two giant planets discovered with this technique.</p>
https://doi.org/10.5281/zenodo.7255841
oai:zenodo.org:7255841
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7255840
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
astrometry
radio astronomy
binaries
young stars
exoplanets
vlbi
Astrometric companions: low-mass stars, brown-dwarfs and planets
info:eu-repo/semantics/conferencePoster
oai:zenodo.org:7246065
2022-10-25T18:49:29Z
openaire
user-vltihow2022
German Chaparro
2022-10-24
<p>Presentation for my invited lecture on protoplanetary disks for VLTI-HOW, ESO Vitacura, Chile, Oct 10-21 http://www.eso.org/sci/meetings/2022/VLTI-How.html</p>
https://doi.org/10.5281/zenodo.7246065
oai:zenodo.org:7246065
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7246064
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
Introduction to Protoplanetary Disks: Theory, Observations and Current Challenges
info:eu-repo/semantics/lecture
oai:zenodo.org:7351284
2022-11-23T14:26:30Z
openaire
user-vltihow2022
Mella, Guillaume
Bourgès, Laurent
2022-11-23
<p>OIFitsExplorer is the JMMC tool to explore your interferometric observations reduced data.</p>
https://doi.org/10.5281/zenodo.7351284
oai:zenodo.org:7351284
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7351283
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
OIFitsExplorer
info:eu-repo/semantics/lecture
oai:zenodo.org:7549044
2023-01-20T02:26:55Z
openaire
user-vltihow2022
Messias, Hugo
2023-01-18
<p>Being at opposite sides of the IT regime, VLTI and ALMA are quite complementary in describing the Universe in different science topics. This presentation goes first through a brief description of ALMA and then shows the different scientific results that gained from the complementarity of these two facilities (proto-planetary discs, extra-solar planets, active galactic nuclei, young stellar objects, asymptotic giant branch stars). The final part of the presentation is all about what future holds, from the Wideband Sensitivity Upgrade and Band 1 at ALMA, to the VLTI+ wide and deep capabilities that will revolutionize our understanding on the covered topics.</p>
https://doi.org/10.5281/zenodo.7549044
oai:zenodo.org:7549044
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7549043
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
VLTI and ALMA Synergies
info:eu-repo/semantics/lecture
oai:zenodo.org:7513048
2023-01-09T12:46:31Z
openaire
user-vltihow2022
de Gregorio-Monsalvo, Itziar
de Gregorio-Monsalvo, Itziar
2023-01-07
<p>In this talk general guidelines for preparing and giving scientific presentations are provided. Different aspects starting with the question on "why giving talks in astronomy?" are considered. Different type of audience, slides design, and talk structure are also discussed. The talk finish with some tips on performance aspects.</p>
https://doi.org/10.5281/zenodo.7513048
oai:zenodo.org:7513048
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7513047
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
scientific presentations
talks
Scientific presentations
info:eu-repo/semantics/lecture
oai:zenodo.org:7308418
2022-11-10T14:26:25Z
openaire
user-vltihow2022
Sergio Sánchez-Sanjuan
2022-11-09
<p>Star formation is a current relevant and active field that involves a wide range of physical processes on both spatial and time scales. Star formation not only governs the structure and evolution of galaxies, but also it is responsible in the origin of planetary systems.</p>
<p>The study of young stellar clusters, using accurate data from huge sky surveys such as GAIA and SLOAN/APOGEE, gives us strong evidence to identify possible sub-clusters and characterise the kinematic and photospheric properties of each target. After cluster parametrization, all the information acquired can be used to evaluate the dynamical evolution employing computational tools in which we can estimate particular features of the system according to their present conditions.</p>
<p>Here, we briefly present a planned research PhD project in which it is expected to have a better understanding on the formation and early evolution of stellar groups from observations and simulations.</p>
https://doi.org/10.5281/zenodo.7308418
oai:zenodo.org:7308418
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7308417
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
Star formation
Young star cluster
Dynamical simulations
Study of Young Stellar Clusters and their dynamical evolution
info:eu-repo/semantics/conferencePoster
oai:zenodo.org:7535093
2023-01-14T02:26:31Z
openaire
user-vltihow2022
Tristram, Konrad R. W.
2023-01-13
<p>Presentation of the results obtained by optical and infrared interferometry on Active Galactic Nuclei (AGN), especially from the Very Large Telescope Interferometer (VLTI). The presentation covers both continuum measurements of sizes, of radial brightness distributions and elongations, of detailed imaging studies, of variability, and of dust parallaxes, as well as spectro-interferometry of emission lines in the broad line region.</p>
https://doi.org/10.5281/zenodo.7535093
oai:zenodo.org:7535093
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7535092
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
AGN
interferometry
The VLTI view on Active Galactic Nuclei
info:eu-repo/semantics/lecture
oai:zenodo.org:7535113
2023-01-14T02:26:39Z
openaire
user-vltihow2022
Tristram, Konrad R. W.
2023-01-13
<p>Description of the near-infrared interferometric instrument GRAVITY at the Very Large Telescope Interferometer, including the instrument layout, technical components, limiting magnitudes, observing modes and resulting data.</p>
https://doi.org/10.5281/zenodo.7535113
oai:zenodo.org:7535113
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7535112
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
interferometry
GRAVITY -- Instrument description
info:eu-repo/semantics/lecture
oai:zenodo.org:7501741
2023-01-04T14:26:25Z
openaire
user-vltihow2022
Nowak, Mathias
2023-01-03
<p>An introduction to how astrometric measurements are done with long-baseline optical interferometry, in single or dual-field, and in particular with the GRAVITY instrument.</p>
https://doi.org/10.5281/zenodo.7501741
oai:zenodo.org:7501741
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7501740
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
Astrometry
info:eu-repo/semantics/lecture
oai:zenodo.org:7250212
2022-10-26T02:26:22Z
openaire
user-vltihow2022
Trisha Bhowmik
2022-10-25
<p>[BHB2007]-1 is an accreting young stellar object which is surrounded by a protoplanetary disk with an enormous gap (~70 au wide). This cavity might have been carved by a very young brown dwarf candidate present at a distance of 0''.32. To date, the presence of this candidate has only been detected in the radio (VLA) and NACO's L' filter, limiting to constrain the mass accurately. </p>
<p>We have GRAVITY observing time to extract the K-band spectrum of the companion candidate for the first time. We aim to constrain the dynamical mass of the companion, characterize it with atmospheric models and perform high-precision astrometry to constrain its position. A successful observation would confirm the presence of the brown dwarf companion candidate. Additionally, we also would be able to observe the circumplanetary environment with a much higher resolution compared to the previous observations.</p>
https://doi.org/10.5281/zenodo.7250212
oai:zenodo.org:7250212
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7250211
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
protoplanetary disk
young stellar object
brown dwarf
Detecting a brown dwarf around a YSO BHB2007-1 with GRAVITY
info:eu-repo/semantics/conferencePoster
oai:zenodo.org:7507025
2023-01-06T14:26:40Z
openaire
user-vltihow2022
Ohnaka, Keiichi
2023-01-05
<p>Mass loss plays an important role in the evolution of massive stars. High angular resolution observations of the atmosphere, wind, and circumstellar environment of evolved massive stars allow us to improve our understanding of the mass-loss mechanism. We review recent results of high angular resolution observations of massive stars in their late evolutionary stages.</p>
https://doi.org/10.5281/zenodo.7507025
oai:zenodo.org:7507025
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7507024
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
VLTI view on evolved massive stars
info:eu-repo/semantics/lecture
oai:zenodo.org:7350843
2022-11-23T14:26:30Z
openaire
user-vltihow2022
Mella, Guillaume
Bourgèsl, Laurent
Tallon-Bosc, Isabelle
Tallon, Michel
2022-11-23
<p> The JMMC is the french center for optical interferometry. It aims at providing support for the users of the stellar interferometers currently in operation. This support is possible thanks to the development of efficient and using friendly tools for preparing the observations, analysing the data or archiving the results. The tools are accessible through the web site and linked to a "Face to Face" help especially for the preparation of observations, the PIONIER, GRAVITY and MATISSE data reduction, and the data analysis.</p>
https://doi.org/10.5281/zenodo.7350843
oai:zenodo.org:7350843
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7350842
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
JMMC Tools
info:eu-repo/semantics/lecture
oai:zenodo.org:7501761
2023-01-04T14:26:33Z
openaire
user-vltihow2022
Nowak, Mathias
2023-01-03
<p>An introduction to some of the main results obtained with the VLTI instruments on exoplanet science, focusing in particular to the contribution made by GRAVITY to the observation and characterization of young giant planets and their atmospheres.</p>
https://doi.org/10.5281/zenodo.7501761
oai:zenodo.org:7501761
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7501760
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
The VLTI view on exoplanets
info:eu-repo/semantics/lecture
oai:zenodo.org:7514098
2023-01-09T12:46:30Z
openaire
user-vltihow2022
de Oliveira, Natanael
Menéndez-Delmestre, Karín
Gonçalves, Thiago
2023-01-08
<p>Recent estimates indicate that dark matter represents 85% of the total matter in the Universe. Its presence, so far, is manifested through gravitational effects, where one of its most concrete evidence can be verified through the rotation curves of disk galaxies. Motivated to understand how dark matter is distributed in galaxies like our own, we define a sample of Milky Way (MW) analog galaxies. Our sample is derived from the S4G and VIVA surveys, which are the most complete surveys regarding stellar mass characterization and atomic hydrogen gas (HI) distribution in nearby galaxies, respectively. The mid-infrared imaging at 3.6 and 4.5μm of the S4G survey is the best single band tracer of the stellar mass, allowing us to make a careful analysis of the baryonic mass distribution in our sample. On the other hand, using the data cubes of the HI distribution from the VIVA survey allows us to map the distribution of the dark matter component. Our sample is composed of 6 MW analogs, defined as such based on the maximum rotation velocity of the HI gas and morphological type similar to the Milky Way. This proves to be efficient as we limit ourselves to objects that present physical characteristics similar to the Milky Way galaxy. For each object present in the sample, we constructed rotation curves from the intensity and velocity maps of the HI derived through the VIVA survey data cubes. In order to disentangle the contributions due to baryonic and dark matter, we did the characterization of the stellar mass distribution based on the S4G imaging. Finally, we develop an analytical model for dark matter distribution and decompose the rotation curves into the different mass contributions. The model is guided by parameters extracted from the decomposition of stellar mass into different components of the internal structure of galaxies (e.g. bulge, disk and halo), ensuring a reliable profile of the mass distribution. This work allows us to generate maps of dark matter distribution in Milky Way analog galaxies, opening the possibility of constructing a set of realistic variations of dark matter profiles in our own galaxy.</p>
https://doi.org/10.5281/zenodo.7514098
oai:zenodo.org:7514098
ang
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7514097
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
vltihow2022, VLTI-How: The VLTI High angular resolution Observations Workshop, ESO Santiago, Chile, October 10-21, 2022
Local dark matter density
Dark matter
Analogs
Rotation curves
Rotation Curve decomposition in Search for a Dark Matter Model for Analog Galaxies
info:eu-repo/semantics/conferencePoster
oai:zenodo.org:7246446
2022-10-25T18:49:59Z
user-vltihow2022
Rojas Lobos, P. Andrea
2022-10-24
<p>A schematic of the AGN and the main source of linear polarization in the optical and UV range, the scattering, both from the continuum and from the broad lines, is shown. Some examples of potential uses of linear polarimetry are presented, such as the observation of broad lines in type 2 AGNs, the measurement and structure of the BLR, a new method to measure the mass of supermassive black holes, and binary supermassive black hole models.</p>
<p> </p>
https://doi.org/10.5281/zenodo.7246446
oai:zenodo.org:7246446
eng
Zenodo
https://zenodo.org/communities/vltihow2022
https://doi.org/10.5281/zenodo.7246445
info:eu-repo/semantics/restrictedAccess
VLTI-How, The VLTI High angular resolution Observations Workshop, ESO-Chile, 10 - 21 October 2022
AGN
Polarimetry
Scattering
Linear Polarization in AGN
info:eu-repo/semantics/conferencePoster