2nd BINA Workshop

9 Oct 2018, 09:00 → 12 Oct 2018, 18:00 UTC

Meridian Room (Royal Observatory of Belgium)

Joan Vandekerckhove (Royal Observatory of Belgium), Peter De Cat (Royal Observatory of Belgium)

Book of Abstracts 18bina_BookOfAbstracts.pdf

Pictures

• 18bina_Picture_DSC0004_OC02.jpg
• 18bina_Picture_DSC0005_OC03.jpg
• 18bina_Picture_DSC0006_OC04.jpg
• 18bina_Picture_DSC0008_IR01.jpg
• 18bina_Picture_DSC0009_IR02.jpg
• 18bina_Picture_DSC0011_IR04.jpg
• 18bina_Picture_DSC0012_IR05.jpg
• 18bina_Picture_DSC0013_CT01.jpg
• 18bina_Picture_DSC0015_RT01.jpg
• 18bina_Picture_DSC5111_CT02.jpg
• 18bina_Picture_DSC5115.jpg
• 18bina_Picture_DSC5118_IR07.jpg
• 18bina_Picture_DSC5122_CT03.jpg
• 18bina_Picture_DSC5126.jpg
• 18bina_Picture_DSC5130_CT04.jpg
• 18bina_Picture_DSC5133_CT05.jpg
• 18bina_Picture_DSC5135.jpg
• 18bina_Picture_DSC5139_CT05.jpg
• 18bina_Picture_DSC5142_CT06.jpg
• 18bina_Picture_DSC5147_CT09.jpg
• 18bina_Picture_DSC5149_IT01.jpg
• 18bina_Picture_DSC5151_CT10.jpg
• 18bina_Picture_DSC5154_CT13.jpg
• 18bina_Picture_DSC5158.jpg
• 18bina_Picture_DSC5159_CT15.jpg
• 18bina_Picture_DSC5165.jpg
• 18bina_Picture_DSC5167.jpg
• 18bina_Picture_DSC5168.jpg
• 18bina_Picture_DSC5174.jpg
• 18bina_Picture_DSC5178_IR09.jpg
• 18bina_Picture_DSC5181_IR09.jpg
• 18bina_Picture_DSC5189_IR10.jpg
• 18bina_Picture_DSC5193.jpg
• 18bina_Picture_DSC5197_CT18.jpg
• 18bina_Picture_DSC5201_CT19.jpg
• 18bina_Picture_DSC5202_CT19.jpg
• 18bina_Picture_DSC5204_CT20.jpg
• 18bina_Picture_DSC5234.jpg
• 18bina_Picture_DSC5245.jpg
• 18bina_Picture_DSC5258.jpg
• 18bina_Picture_DSC5259.jpg
• 18bina_Picture_DSC5261.jpg
• 18bina_Picture_DSC5264_CT21.jpg
• 18bina_Picture_DSC5265_CT21.jpg
• 18bina_Picture_DSC5270_CT23.jpg
• 18bina_Picture_DSC5281.jpg
• 18bina_Picture_DSC5285.jpg
• 18bina_Picture_DSC5286.jpg
• 18bina_Picture_DSC5291_CT27.jpg
• 18bina_Picture_DSC5301_CT28.jpg
• 18bina_Picture_DSC5304_CT29.jpg
• 18bina_Picture_DSC5307.jpg
• 18bina_Picture_DSC5313.jpg
• 18bina_Picture_DSC5316.jpg
• 18bina_Picture_DSC5320.jpg
• 18bina_Picture_DSC5322.jpg
• 18bina_Picture_DSC5325_IR11.jpg
• 18bina_Picture_DSC5328_CT31.jpg
• 18bina_Picture_DSC5330.jpg
• 18bina_Picture_DSC5332.jpg
• 18bina_Picture_DSC5334.jpg
• 18bina_Picture_DSC5335.jpg
• 18bina_Picture_DSC5336.jpg
• 18bina_Picture_DSC5363_CS04.jpg
• 18bina_Picture_Workshop.jpg
• 18bina_Picture_WorkshopWithNames.jpg

Poster 18bina_Affiche.jpg

Scientific programme 18bina_ScientificProgramme.pdf

Slides

• 18bina_Presentation_CT01_Raskin.pdf
• 18bina_Presentation_CT02_OrbandeXivry.pdf
• 18bina_Presentation_CT03_Pradhan.pdf
• 18bina_Presentation_CT04_JoshiY.pdf
• 18bina_Presentation_CT05_Lampens.pdf
• 18bina_Presentation_CT06_Singh.pdf
• 18bina_Presentation_CT08_Yadav.pdf
• 18bina_Presentation_CT10_Naik.pdf
• 18bina_Presentation_CT11_KoonammakkilGeorge.pdf
• 18bina_Presentation_CT13_Sluse.pdf
• 18bina_Presentation_CT14_Mandal.pdf
• 18bina_Presentation_CT15_Dubey.pdf
• 18bina_Presentation_CT16_Sharma.pdf
• 18bina_Presentation_CT18_Veerappa.pdf
• 18bina_Presentation_CT20_Semenko.pdf
• 18bina_Presentation_CT23_Jameela.pdf
• 18bina_Presentation_CT24_Tej.pdf
• 18bina_Presentation_CT25_Das.pdf
• 18bina_Presentation_CT27_JoshiS.pdf
• 18bina_Presentation_CT29_DeBecker.pdf
• 18bina_Presentation_CT31_Decleir.pdf
• 18bina_Presentation_CT32_Gupta.pdf
• 18bina_Presentation_IR01_Ribas.pdf
• 18bina_Presentation_IR02_Pasquali.pdf
• 18bina_Presentation_IR04_Ramaprakash.pdf
• 18bina_Presentation_IR05_VanWinckel.pdf
• 18bina_Presentation_IR06_Pandey.pdf
• 18bina_Presentation_IR08_Sagar.pdf
• 18bina_Presentation_IR09_Jehin.pdf
• 18bina_Presentation_IR10_Chenakkod.pdf
• 18bina_Presentation_IR11_Baes.pdf
• 18bina_Presentation_IR12_Prugniel.pdf
• 18bina_Presentation_OC02_JoshiS.pdf
• 18bina_Presentation_OC03_Freire.pdf
• 18bina_Presentation_P01_DeBecker.pdf
• 18bina_Presentation_P04_Ghosh.pdf
• 18bina_Presentation_P06_Singh.pdf
• 18bina_Presentation_P07_Bharti.pdf

Venue 18bina_Venue.pdf

Video

• 18bina_Presentation_CT02_OrbandeXivry.mp4
• 18bina_Presentation_CT03_Pradhan.mp4
• 18bina_Presentation_CT04_JoshiY.mp4
• 18bina_Presentation_CT05_Lampens.mp4
• 18bina_Presentation_CT07_Mondal.mp4
• 18bina_Presentation_CT09_Mazumdar.mp4
• 18bina_Presentation_CT10_Naik.mp4
• 18bina_Presentation_CT11_KoonammakkilGeorge.mp4
• 18bina_Presentation_CT12_Dabhade.mp4
• 18bina_Presentation_CT13_Sluse.mp4
• 18bina_Presentation_CT14_Mandal.mp4
• 18bina_Presentation_CT15_Dubey.mp4
• 18bina_Presentation_CT16_Sharma.mp4
• 18bina_Presentation_CT17_Karmakar.mp4
• 18bina_Presentation_CT18_Veerappa.mp4
• 18bina_Presentation_CT23_Jameela.mp4
• 18bina_Presentation_CT24_Tej.mp4
• 18bina_Presentation_CT25_Das.mp4
• 18bina_Presentation_CT27_JoshiS.mp4
• 18bina_Presentation_CT29_DeBecker.mp4
• 18bina_Presentation_CT30_Khata.mp4
• 18bina_Presentation_CT31_Decleir.mp4
• 18bina_Presentation_IR01_Ribas.mp4
• 18bina_Presentation_IR04_Ramaprakash.mp4
• 18bina_Presentation_IR07_Ganesh.mp4
• 18bina_Presentation_IR08_Sagar.mp4
• 18bina_Presentation_IR09_Jehin.mp4
• 18bina_Presentation_IR10_Chenakkod.mp4
• 18bina_Presentation_IR11_Baes.mp4
• 18bina_Presentation_OC02_JoshiS.mp4
• 18bina_Presentation_OC03_Freire.mp4

Tuesday, 9 October

08:30 → 09:00 Start of day 1 (Meridian Room opens)

09:00 → 09:45 Registration

09:45 → 10:30 Opening ceremony

09:45 Welcome

Speaker: Dr Ronald Van der Linden (Royal Observatory of Belgium)

09:55 Belgo-Indian Network for Astronomy & Astrophysics (BINA)

Speaker: Dr Santosh Joshi (ARIES, Nainital)

Slides 18bina_Presentation_OC02_JoshiS.pdf

Video 18bina_Presentation_OC02_JoshiS.mp4

10:05 The Belgian Science Policy Office (BELSPO)

Speaker: Ms Margarida Freire (Belgian Science Policy (BELSPO))

Pictures 18bina_Picture_DSC0005_OC03.jpg

Slides 18bina_Presentation_OC03_Freire.pdf

Video 18bina_Presentation_OC03_Freire.mp4

10:15 Advanced Mechanical & Optical Systems (AMOS)

Speaker: Dr Xavier Verians (Advanced Mechanical & Optical Systems (AMOS))

Pictures 18bina_Picture_DSC0006_OC04.jpg

10:30 → 11:10 1. Instrumentation of the Indo-Belgian Telescopes

10:30 Astrophysics and exoplanets with a 4-m class telescope

I will review current and future plans for instrumentation of 4-m telescopes. The focus of the talk will be on those instruments relevant to stellar astrophysics and exoplanet science and, particularly, on high-resolution spectroscopy. I will describe the experience of CARMENES and similar instruments and put it in the context of transiting exoplanet searches from space such as the TESS and PLATO missions.

Speaker: Dr Ignasi Ribas (Institut de Ciencies de l'Espai (CSIC) & IEEC)

Pictures 18bina_Picture_DSC0008_IR01.jpg

Slides 18bina_Presentation_IR01_Ribas.pdf

Video 18bina_Presentation_IR01_Ribas.mp4

11:10 → 11:40 Coffee/Tea break

11:40 → 13:00 1. Instrumentation of the Indo-Belgian Telescopes

11:40 The far-reaching impact of surveys carried out with 4m-class telescopes

The goal of my presentation is to give a panoramic view of imaging/spectroscopic surveys conducted at 4m-class telescopes during recent years. Special emphasis and discussion are given to the results obtained by extragalactic surveys on galaxy evolution.

Speaker: Dr Anna Pasquali (Astronomisches Rechen-Institut)

Pictures 18bina_Picture_DSC0009_IR02.jpg

Slides 18bina_Presentation_IR02_Pasquali.pdf

12:20 Performance of the instruments on 3.6-m Devasthal Optical Telescope

The 3.6-m Devasthal Optical Telescope (DOT) is being utilised with a 4Kx4K vis-CCD (IMAGER) and a near-infrared array (TIRCAM) in imaging mode, and a Faint Object Spectrograph & Camera (FOSC)-type instrument (in commissioning stage) in spectroscopy+imaging mode using a 4Kx4K vis-CCD camera. This talk will summarise the ​global ​performance of some instruments used with the DOT.

Speaker: Dr Amitesh Omar (ARIES)

13:00 → 14:30 Lunch break

14:30 → 16:10 1. Instrumentation of the Indo-Belgian Telescopes

14:30 Current and future science instruments for the 3.6-m Devasthal Optical Telescope

A number of instruments have been or are being built for the 3.6-m Devasthal Optical Telescope. These include the Imager, ADFOSC, TANSPEC, DOTIFS, etc. This invited talk will provide a review of these instruments covering their capabilities, current status and main science drivers. The talk will also mention some ideas for future instrumentation that were discussed in various forums.

Speaker: Prof. Anamparambu Ramaprakash (IUCAA)

Pictures 18bina_Picture_DSC0011_IR04.jpg

Slides 18bina_Presentation_IR04_Ramaprakash.pdf

Video 18bina_Presentation_IR04_Ramaprakash.mp4

15:10 10 years of HERMES at the 1.2-m Mercator telescope

In this contribution I will review our approach to exploiting a small but flexible 1.2-m Mercator telescope. Its specific niche in observational astrophysics needs both a instrument development programme, a continuous technical development programme and an optimised operational model. I will review the 'lessons learned' from our exploitation of the high-resolution HERMES spectrograph mounted on the telescope in 2009.

Speaker: Prof. Hans Van Winckel (KU Leuven)

Pictures 18bina_Picture_DSC0012_IR05.jpg

Slides 18bina_Presentation_IR05_VanWinckel.pdf

15:50 Upgrading HERMES: an improved fiber link and a new wavelength calibrator

After nearly ten years of successful operations, HERMES, the fibre-fed high-resolution spectrograph of the Mercator telescope is currently being upgraded. We are equipping it with a new optical fibre link and a new wavelength calibration system is under development. Three measures will increase the radial-velocity (RV) performance of the fibre link. The use of octagonal instead of circular core fibres and imaging the stellar image instead of the telescope pupil on the fibre entrance, will both help to improve the illumination stability of the spectrograph. Furthermore, the new fibre link will also allow to observe, simultaneously with the high-resolution stellar spectrum, a wavelength reference source. This makes it possible to track any instrumental drift during the exposure. High-accuracy RV measurements require very precise wavelength calibration. To overcome the insufficiencies of the standard Thorium-argon emission lamps, we are developing a wavelength calibration system based on a Fabry-Perot etalon. Illuminated with a white-light source, the etalon provides a dense comb spectrum with very regular spacing and amplitude. Using laser spectroscopy to anchor the etalon spectrum to a precisely known hyperfine transition of Rubidium, delivers sub-m/s stability over time scales of years. Both developments will increase the RV accuracy of the HERMES spectrograph and could also be of great benefit for the future high-resolution spectrograph on the DOT@ARIES telescope.

Speaker: Dr Gert Raskin (KU Leuven)

Pictures 18bina_Picture_DSC0013_CT01.jpg

Slides 18bina_Presentation_CT01_Raskin.pdf

16:10 → 16:30 Coffee/Tea break

16:30 → 18:10 1. Instrumentation of the Indo-Belgian Telescopes: Round-table discussion

16:30 The High Resolution Spectrograph of the Aryabhatta Research Institute of Observational Sciences

A high resolution spectrograph for recently installed 3.6-m Devasthal Optical Telescope (DOT) of the Aryabhatta Research Institute of Observational Sciences (ARIES) is envisaged as a key instrument to meet the spectroscopic requirements of the telescope. A committee of national and international experts recommended the key science program that can be taken up with the proposed instrument as asteroseisomology, Doppler imaging of spotted stars, abundances studies, spectroscopy and ground-based follow-up of exoplanets, and supernovae. The committee recommends the technical specification of the proposed instrument as follows: two mode of spectral resolution (40k and 80k), spectral coverage of 380-900 nm, and high throughput of ~20%. Further, the spectrograph should be able to record simultaneously the spectra of an object and/or sky. The spectrograph would be mounted on a vibration isolation table in a temperature controlled environment. The instrument has a fixed configuration with no moving parts ensuring a robust operation and easy maintenance. I aim to present current status of the proposed spectrograph during the talk.

Speaker: Dr Jeewan Pandey (Aryabhatta Research Institute of Observational Sciences)

Slides 18bina_Presentation_IR06_Pandey.pdf

17:10 Round table discussion

Pictures 18bina_Picture_DSC0015_RT01.jpg

18:10 → 18:40 End of day 1 (Meridian Room closes)

Wednesday, 10 October

09:00 → 09:30 Start of day 2 (Meridian Room opens)

09:30 → 09:50 1. Instrumentation of the Indo-Belgian Telescopes

09:30 A sharp future for the 3.6-m Devasthal Optical Telescope? The power of adaptive optics for medium size telescopes

Adaptive optics (AO), by compensating in real time the blurring due to atmospheric turbulence, improves the angular resolution and the sensitivity of ground-based telescopes. AO represents an opportunity for medium size telescopes to be competitive with respect to large and very large observatories, either by being highly automatized and allowing high-yield surveys to be undertaken, or by providing very high correction up to visible wavelengths. More generally, AO can be beneficial for most scientific cases and - we think - reachable with a moderate effort investment. In this contribution, I will present the expertise we are currently building up in Liège with the SALTO project, a 1-m telescope with laser guided adaptive optics system. I will then focus on two different sciences cases, discuss how they would drive the design of the AO system, and the general benefit that AO would bring to the 3.6-m Devasthal Optical Telescope (DOT).

Speaker: Dr Gilles Orban de Xivry (University of Liège)

Pictures 18bina_Picture_DSC5111_CT02.jpg

Slides 18bina_Presentation_CT02_OrbandeXivry.pdf

Video 18bina_Presentation_CT02_OrbandeXivry.mp4

09:50 → 10:50 2. Data & Science with the Indo-Belgian telescopes: 1. Solar system and exoplanet studies with the Indo-Belgian telescopes

09:50 Solar system studies with the Indo-Belgian Telescopes

Access to 2 and 4m class telescopes and sophisticated instrumentation are one of the key points of the BINA collaboration. It is expected that like other fields, the field of solar system astronomy would also greatly benefit from observations carried out with these telescopes. In this review talk I will be highlighting some of the work carried out on similar telescopes elsewhere and the gap areas that could be filled with the use of instruments that are now becoming available on the telescopes available to the BINA collaboration. It is expected that our understanding of the solar system bodies, particularly the minor bodies and other smaller objects, would be greatly enhanced in terms of statistics as well as detailed characterization of individual ones. It is also important to have a full characterization and understanding of the potentially hazardous asteroids in the vicinity of the Earth's orbit. They are generally fainter than 18th magnitude and not easily observable with the smaller telescopes. This talk will summarize the current status of the field and discuss possible science cases with the new facilities.

Speaker: Dr Shashikiran Ganesh (Physical Research Laboratory, Ahmedabad, India)

Pictures 18bina_Picture_DSC5118_IR07.jpg

Video 18bina_Presentation_IR07_Ganesh.mp4

10:30 Size estimation of orbital debris using a zenith-pointing telescope

The size distribution of space debris is an important input to risk analysis for current and future space missions. In preparation for future observations with the zenith-pointing 4-m International Liquid Mirror Telescope, the 1.3-m Devasthal Fast Optical Telescope was used to gain experience with zenith-pointing observations and, serendipitously, to detect, identify and characterize orbital debris. Observational data were acquired on 11 nights in May, 2015 using a 2048 $\times$ 2048-pixel CCD detector operating in time-delay integration mode. Twelve moving objects were detected, mostly during dawn and twilight. All were identified by correlation with two-line element sets. By modeling each of the objects as a diffuse Lambertian sphere with an albedo of 0.175, their effective diameters were estimated from the observed apparent magnitudes, altitudes, velocities and solar phase angles. Seven objects were found to be in low Earth orbit and five in mid-Earth or geo-transfer orbits. The apparent Gaia magnitudes of the identified objects range from 5.6 to 12.0 and the estimated effective diameters from 0.3 to 10.1 m. Images from the future ILMT photometric survey are expected to provide detections of objects having diameters as small as 3 cm in low-Earth orbit.

Speaker: Mr Bikram Pradhan (University of Liège)

Pictures 18bina_Picture_DSC5122_CT03.jpg

Slides 18bina_Presentation_CT03_Pradhan.pdf

Video 18bina_Presentation_CT03_Pradhan.mp4

10:50 → 11:30 2. Data & Science with the Indo-Belgian telescopes

10:50 Scientific potential of Indo-Belgian 3.6 m DOT and ILMT in the field of Galactic Astronomy

Both India and Belgium have jointly established two 4 meter class optical telescopes at Devasthal, Nainital (Longitude = 79º 41' 04" E; Latitude = 29 º 21' 40" N; Altitude= 2450 m) located in central Himalayan region of Kumaon, Uttarakhand, India. After successful installation of the 3.6 meter modern new technology Devasthal Optical Telescope (DOT) in 2015, it was technically activated by premiers of both countries from Brussels on March 30, 2016 while first light from 4 meter International Liquid Mirror Telescope (ILMT) is expected soon. Since 2016, the 3.6 m DOT has been used for both optical and near-Infrared (NIR) observations for a number of research proposals submitted primarily from astronomers of India and Belgium. The best recorded value of angular resolution is 0.4 arc second indicating that the optics of the 3.6 m DOT telescope is good and capable of providing images of the celestial bodies with sub arc second resolutions. All these observations provide proof that the care taken during the construction of the telescope houses has paid a rich dividend as their thermal mass is so low that it has not degraded the natural atmospheric seeing at Devasthal measured about 2 decades ago during 1997 – 1999 using differential image motion monitor. A few preliminary scientific results obtained from recent observations will be presented in this review talk along with performance and global potential of the 3.6 m DOT in the field of galactic astronomy. The 3.6 m DOT is capable of providing internationally competitive science once high resolution spectrograph and other planned modern backend instruments become operational. Geographical location of the observatory has global importance for the time domain and multi-wavelength astrophysical studies. Both 4-m class observing facilities located at Devasthal have enormous potential as they can provide valuable optical and NIR observations for a number of front line galactic astrophysical research problems.

Speaker: Prof. Ram Sagar (Indian Institute of Astrophysics)

Slides 18bina_Presentation_IR08_Sagar.pdf

Video 18bina_Presentation_IR08_Sagar.mp4

11:30 → 11:50 Coffee/Tea break

11:50 → 13:10 2. Data & Science with the Indo-Belgian telescopes: 2. Galactic astronomy with the Indo-Belgian telescopes

11:50 Optical characterization and radial velocity monitoring of exoplanet and eclipsing binary candidates

Recently, large catalogues of exoplanet and eclipsing binary candidates are reported in the Kepler archival data. In the framework of BINA, we therefore initiated a long-term project "Optical characterization and Radial velocity monitoring with Belgian and Indian Telescopes (ORBIT)" which focuses on ground-based photometric monitoring and high-resolution spectroscopic observations of selected exoplanet candidates and low-mass eclipsing binary candidates using the Indo-Belgian telescopes. We initially focus our study on few bright candidates for which radial velocity monitoring could be possible from the recently mounted high-resolution spectrograph on 2-m Himalayan Chandra Telescope (HCT). Along with planned photometric observations using small-size telescopes at ARIES, Nainital, we aim to determine their physical parameters with a great precision. Having enough sample off such low-mass objects, we aim to understand their mass-radius characteristic which is still debated towards the lower-mass regime. Furthermore, if a transit occurs during the period of spectroscopic observations, it may also help to monitor the Rossiter-McLaughlin effect which plays an important role in the understanding of the characteristics of the secondary star, particularly in the case of a low-mass star or planetary companion.

Speaker: Dr Yogesh Joshi (Scientist ARIES)

Pictures 18bina_Picture_DSC5130_CT04.jpg

Slides 18bina_Presentation_CT04_JoshiY.pdf

Video 18bina_Presentation_CT04_JoshiY.mp4

12:10 Eclipse mapping of Algol-type systems with oscillating $\delta$ Scuti type components

The oEA stars are the former secondaries of evolved, semi-detached eclipsing binaries which are (still) undergoing mass transfer and form a newly detected class of pulsators close to the main sequence (Mkrtichian et al. 2002). Their unique feature consists of mass accretion onto the atmosphere of the pulsating star. Mass accretion affects the mass, radius, density as well as the star's evolution (depending on the accretion rate). Such stars are therefore very attractive targets for asteroseismic studies. The eclipse mode identification method for EBs with pulsating components was suggested by Nather & Robinson (1974). The method uses the primary eclipse event as a spatial filter to resolve the pulsations across the stellar surface of the pulsator. It is based on the fact that, during an eclipse of the pulsating component, the occulting star acts as a screen with a timely variable shape. During an eclipse, depending on the (l,m) spatial structure of modes, different shapes of the pulsation amplitude and phase variations are observed. A comparison between the modelled and the observed amplitude and phase patterns provides the correct mode identification. The method (also called dynamic eclipse mapping method; Bíró et al. 2011) needs a geometrical model, pulsation frequencies as well as the light curves as input. The geometrical model can be obtained from a simultaneous modelling of the light (photometry) and radial velocity curves (acquired with the HERMES spectrograph). The pulsation frequencies are obtained from subtracting a binary model from the original light curves followed by a frequency analysis of the residuals. We will identify and illustrate systems where observations with a (relatively) fast CCD camera equipping the 3.6-m Devasthal Optical Telescope (DOT) could deliver the data needed for the application of the eclipse mapping method.

Speaker: Dr Patricia Lampens (Koninklijke Sterrenwacht van België)

Pictures 18bina_Picture_DSC5133_CT05.jpg 18bina_Picture_DSC5139_CT05.jpg

Slides 18bina_Presentation_CT05_Lampens.pdf

Video 18bina_Presentation_CT05_Lampens.mp4

12:30 Light curve parameters of Cepheid and RR Lyrae variables at multiple wavelengths: theory vs. observations

We analyse the theoretical light curves of Cepheid and RR Lyrae variables at optical (UBVRI) and near-infrared (JKL) wavelengths using Fourier decomposition. A large number of models have been studied appropriate for galactic and magellanic cloud Cepheids and RR Lyraes. We discuss the variation of light-curve parameters with different compositions and mass-luminosity levels as a function of period and wavelength, and compare our results with observations.

Speaker: Prof. Harinder P. Singh (University of Delhi)

Pictures 18bina_Picture_DSC5142_CT06.jpg

Slides 18bina_Presentation_CT06_Singh.pdf

12:50 Rotation rates of pre-main sequence stars

Pre-main sequence (PMS) stars first came into the spotlight due to their photometric variable characteristics. Observational studies have been performed on exploring variability in young stars and the role of angular momentum in their stellar evolution. The variability in a PMS star is thought to be originated via various mechanisms like magnetically induced cool spots or magnetically channelled variable accretion flows generating hot spots on the star surface, eclipsing binary, opacity due to non-uniform dust distribution, etc. In this presentation, we like to highlight some of our results on the variability of young stellar objects in a few galactic star-forming regions.

Speaker: Dr Soumen Mondal (S. N. Bose National Centre for Basic Sciences)

Video 18bina_Presentation_CT07_Mondal.mp4

13:10 → 14:30 Lunch break

14:30 → 15:10 2. Data & Science with the Indo-Belgian telescopes: 2. Galactic astronomy with the Indo-Belgian telescopes

14:30 Instabilities and mass-loss in massive stars

Spectroscopic and photometric variabilities have been noticed in several stars. The cause and responsible mechanism for such variabilities are not yet properly understood. Among the possible origins, radial and non-radial pulsations have been proposed as a cause of these variabilities. With the help of linear stability analysis, we have found several strong instabilities in models of massive zero age main sequence and post main sequence stars. To find the final fate of the unstable models, we have followed the identified instabilities into the non-linear regime using an energy conservative numerical scheme for selected stellar models. Rearrangement of stellar structure, finite amplitude pulsations (with periods between few hours to several days) and surface eruptions have been noticed as the final consequences of these instabilities. In case of finite amplitude pulsations, our estimates for pulsationally driven mass-loss rates are of the order of 10^{-4} M_sun/year for few massive OB-type stars which can potentially affect the stellar evolution. Observations of massive-luminous stars such as luminous blue variables (LBVs) using BINA telescopes will provide a unique opportunity to test our theoretical predictions of linear stability analysis and non-linear numerical simulations.

Speaker: Dr Abhay Pratap Yadav (University of Goettingen, Germany)

Slides 18bina_Presentation_CT08_Yadav.pdf

14:50 Accurate estimation of effective temperature and metallicity of asteroseismic targets with BINA telescopes

Recent data from the NASA Kepler mission has provided a big boost to asteroseismic studies of solar-type stars and red giants. It is now possible to provide strict constraints to models of such stars by comparing the observed frequencies with the theoretically predicted ones. However, the seismic constraints are only useful when the effective temperature (Teff) and surface metallicity ([Fe/H]) of the observed stars are accurately known. We propose to use the telescopes under the BINA collaboration to obtain high resolution spectroscopy in order to estimate Teff and [Fe/H] of both observed and future Kepler and TESS targets. The possibility of obtaining a colour-temperature calibration curve, using photometric observations with the Devasthal Optical Telescope (DOT) will also be explored.

Speaker: Prof. Anwesh Mazumdar (Homi Bhabha Centre for Science Education)

Pictures 18bina_Picture_DSC5147_CT09.jpg

Video 18bina_Presentation_CT09_Mazumdar.mp4

15:10 → 16:20 2. Data & Science with the Indo-Belgian telescopes: 3. Extragalactic astronomy with the Indo-Belgian telescopes

15:10 The diversity of Active Galactic Nuclei variability: Some highlights and challenges

The talk will mainly focus on the variability patterns of active galactic nuclei (AGN), specially their subset (including quasars, BL Lacs, Seyfert galaxies) which manifests nuclear jets of nonthermal radiation boosted due to relativistic beaming. Many of their striking observational traits, particularly intensity variations have been extensively recorded across the electromagnetic spectrum, on time scales ranging from sub-minute to decades. In contrast, observations of structural changes in their nuclear jets are almost entirely limited to the radio/millimetre waveband, since there alone do we have the capability to image the parsec-scale nuclear structure of AGN. The existing vast amounts of observational material has revealed several interesting trends which contribute richly to the theoretical modeling of the AGN phenomenon. We shall highlight a selection of them and discuss how these intriguing results can be probed deeper using the optical telescopes recently established at Devasthal (Nainital), in addition to the studies using the existing large telescopes operating in the radio and high-energy bands.

Speaker: Prof. GOPAL KRISHNA (ARIES, Nainital)

Pictures 18bina_Picture_DSC5149_IT01.jpg

15:40 Complex X-ray/ultraviolet/optical variabilities of the Seyfert 1 galaxy NGC 4593

We present a detailed multi-frequency analysis of an intense monitoring programme of the Seyfert 1 galaxy NGC 4593 over a duration of nearly a month with the Swift observatory. We used 185 pointings to study the variability in six ultraviolet/optical and two soft (0.3-1.5 keV) and hard X-ray (1.5-10 keV) bands. The amplitude of the observed variability is found to decrease from high energy to low energy (X-ray to optical) bands. Count-count plots of ultraviolet/optical bands with hard X-rays clearly suggest the presence of a mixture of two major components: (i) highly variable component such as hard X-ray emission, and (ii) slowly varying disc-like component. The variations observed in the ultraviolet/optical emission are strongly correlated with the hard X-ray band. Cross-correlation analysis provides the lags for the longer wavelengths compared to the hard X-rays. Such lags clearly suggest that the changes in the ultraviolet/optical bands follow the variations in the hard X-ray band. This implies that the observed variation in longer wavelengths is due to X-ray reprocessing. Though, the measured lag spectrum (lag versus wavelength) is well described by λ^4/3 as expected from the standard disc model, the observed lags are found to be longer than the predicted values from standard disc model. This implies that the actual size of the disc of NGC 4593 is larger than the estimated size of standard thin disc.

Speaker: Dr SACHINDRA NAIK (PHYSICAL RESEARCH LABORATORY, AHMEDABAD, INDIA)

Pictures 18bina_Picture_DSC5151_CT10.jpg

Slides 18bina_Presentation_CT10_Naik.pdf

Video 18bina_Presentation_CT10_Naik.mp4

16:00 Multi-wavelength studies of Zwicky's Nonet

We present the results of our radio, optical and infrared studies of Zwicky's Nonet, which is a compact group of nine merging galaxies, at the centre of the rich galaxy cluster A 407. Here, all the nine galaxies are packed within a radius of only 25 kpc, with the smallest projected separation between galaxy pair combinations is about 5 kpc. This group is found to be hosting a radio source 4C 35.06, which is having helically twisted and kinked radio jets and diffuse outer lobes, revealed by the Giant Meterwave Radio Telescope (GMRT) observations at 610, 235 and 150 MHz frequencies. The host of the radio source is suggested to be a low luminosity galaxy, which might have stripped of its stars in multiple tidal encounters. A consistently observed low-value of the estimated black hole mass from the K-band magnitude compared to that from stellar velocity dispersion for all the galaxies in the sample is pointing to this possibility. Optical and infrared studies show that all the galaxies in the group are of low-excitation class. We have acquired data from 3.6-m Devasthal Optical Telescope (DOT) via some deep observations for this exotic source. Preliminary results are very promising. We will present the multi-wavelength properties of Zwicky's Nonet and discuss the results from the 3.6-m DOT.

Speaker: Mr BIJU KG (WMO Arts \& Science college, Muttil, Kerala, India-673122)

Slides 18bina_Presentation_CT11_KoonammakkilGeorge.pdf

Video 18bina_Presentation_CT11_KoonammakkilGeorge.mp4

16:20 → 16:40 Coffee/Tea break

16:40 → 18:00 2. Data & Science with the Indo-Belgian telescopes: 3. Extragalactic astronomy with the Indo-Belgian telescopes

16:40 Multi-wavelength studies of giant radio galaxies

In this talk, we will present about Giant Radio Galaxies (GRGs) and highlight the importance of their studies and our efforts to solve major standing problems related to growth and evolution of GRGs and their host active galactic nucleus (AGN). They represent an extreme class of active galaxies which have linear sizes in the range of ~0.7 Mpc to 5 Mpc which places them among the largest single astrophysical objects known to us. Over the past four decades, only ~400 GRGs are known as opposed to thousands of radio galaxies (~10-700 Kpc). It is unsettled if the large sizes of GRGs indicate the high efficiency of radio jets ejected from the central AGN, or they grow to enormous sizes due to their location in sparser cluster environments. In spite of various studies of GRGs, there is still not a single tested unified model which might explain the immense physical scale and other extreme properties of GRGs. Moreover, until now only a small fraction of these GRGs have been studied in sufficient detail in multiple wavebands for achieving a good understanding of their unusual nature. This puts a restriction on carrying out statistical studies of their properties. Firstly, under our project SAGAN (Search & Analysis of GRGs with Associated Nuclei), we have successfully made a complete & uniform sample of all known GRGs from literature, which is first of its kind. Secondly, we are also carrying out large-scale searches for new samples of GRGs using existing radio and optical survey data. Thirdly, we plan to study the hosts of GRGs in multi-wavelengths to understand the nature of accretion, feedback and their excitation types. We have already observed some GRGs with the Giant Metrewave Radio Telescope (GMRT) and we plan to observe their host using the 3.6-m Devasthal Optical Telescope to study near-infrared properties of their host galaxies.

Speaker: Mr Pratik Dabhade (IUCAA)

Video 18bina_Presentation_CT12_Dabhade.mp4

17:00 Strong lensing studies with the 3.6-m Devasthal Optical Telescope: opportunities and challenges

Strongly lensed quasars and active galactic nuclei (AGN), namely active galaxies that appear multiply imaged due to a foreground lensing galaxy, are exceptional astrophysical tools that may be used to probe the expansion rate of the Universe, study the evolution of galaxies and of their dark matter content over cosmic time, and zoom in into the structure of AGNs. We are entering a new era in observational astrophysics, not anymore limited by the number of accessible targets, but by our ability to carry out follow-up observations. In this talk, I will present two areas where a spectrograph attached to the 3.6-m Devasthal Optical Telescope (DOT) may yield to important scientific contributions. (1) Discovery of new lensed candidates: A 4-m class telescope is ideal to confirm the nature and derive the basic properties of newly discovered lensed candidates, but also support observations with larger telescope facilities (Very Large Telescope, ALMA, ...). I will expain the scientific importance of such follow-up observations and discuss the number of accessible targets and observational requirements for a successful project. (2) Gravitational microlensing: the stars in the main lensing galaxy act as numerous micro-lenses that magnify the inner regions of AGN, allowing one to uniquely constrain the size and energy profile of the accretion disc. Multi-epochs and low resolution spectroscopy on a 4-m class telescope may constrain the accretion disc structure of tens of AGNs, allowing a breakthrough in the field. We will discuss the motivation and observational challenges associated to such a research project.

Speaker: Dr Dominique Sluse (STAR Institute (U. Liège))

Pictures 18bina_Picture_DSC5154_CT13.jpg

Slides 18bina_Presentation_CT13_Sluse.pdf

Video 18bina_Presentation_CT13_Sluse.mp4

17:20 REMAP: REverberation Mapping of AGN Program at the 2m Himalayan Chandra Telescope

Active galactic nuclei (AGN) are high luminosity sources powered by accretion of matter onto super-massive black holes (SMBHs). According to the unification model of AGN, the SMBH is surrounded by a dusty torus. It is difficult to study the extent of the dusty torus as the central region of AGN is not resolvable using any conventional imaging techniques available today. Though the current optical/infrared interferometric technique could in principle resolve the torus in nearby AGN, it is very expensive. An alternative and cheap method to the interferometric technique to find the extent of the dusty torus is through the technique of reverberation mapping. Towards this we are carrying out a dedicated monitoring program since the year 2016 using the 2-m Himalayan Chandra Telescope (HCT) operated by the Indian Institute of Astrophysics (IIA) in Bangalore (India). Our sample for this program consists of about a dozen sources suitable for observations using the HCT. Observations are routinely carried out once every 5 days to monitor our sample. We have obtained good estimates of the size of the torus in two AGN in our sample. This talk will outline the importance of this program, the observational strategy that is followed, the adopted analysis procedures, the results obtained till now from this program and the scope for Indo-Belgian collaboration.

Speaker: Mr Amit Kumar Mandal (Indian Institute of Astrophysics, CHRIST(Deemed to be University), Bangalore)

Slides 18bina_Presentation_CT14_Mandal.pdf

Video 18bina_Presentation_CT14_Mandal.mp4

17:40 Observations of galaxy collisions and prediction of parameters of resulting galaxies

Galaxy collision is an important event in astrophysics and opens doors for many unanswered questions. The collision between NGC 1232 with a dwarf galaxy or NGC 5256 is another example of merging of two galaxies. APR 256 is another example of merging of the two spiral galaxies. These collisions takes place for millions of years and the statistics changes with time. However, observations show that these events may result in very high temperatures of the order of a few MK, covers and spread over very large areas of the order of few kpc in diameter, and moderate to high luminosity. Depending upon certain factors the collision can be observed under X-RAY band or gamma ray bands. By studying these collisions, the prediction can be made about the shape, size, temperature, expansion, luminous afterglow, etc. of the resulting galaxy. For example, two spiral galaxies can merge to form an elliptical galaxy. The behaviour of present such events can help in predicting the future events.

Speaker: Mr Rajesh Kumar Dubey (Researcher and Principal)

Pictures 18bina_Picture_DSC5159_CT15.jpg

Slides 18bina_Presentation_CT15_Dubey.pdf

Video 18bina_Presentation_CT15_Dubey.mp4

18:00 → 18:20 End of day 2 (Meridian room closes)

Thursday, 11 October

09:00 → 09:30 Start of day 3 (Meridian room opens)

09:30 → 10:10 3. Data & Science with other telescopes of interest: 1. Solar system and exoplanet studies with other telescopes of interest

09:30 Study of small bodies of the Solar System with small and large telescopes

Comets, asteroids and transneptunien objects are remnants of the early stages of the Solar system and, likely, the most pristine solar system bodies. Understanding their nature and their evolution is a clue to the history of our Solar System and panet formation. Comets and meteorites contain complex organic molecules, and may have played a key role in the transfer of water and organics from the interstellar medium to the early Earth, contributing to the origin of life. This interest is well illustrated by the fact that several space missions have targeted small bodies of the solar system in the past years and comets particularly like the very successful ESA Rosetta/Philae mission that returned impressive science data that are changing our knowledge on comets. In this talk I will review the studies we are involved in my group at the STAR institute of the University of Liège using our TRAPPIST robotic small telescope in Chile and Morocco as well as large telescopes as the ESO VLT.

Speaker: Dr Emmanuel Jehin (STAR Institute - University of Liège)

Pictures 18bina_Picture_DSC5178_IR09.jpg 18bina_Picture_DSC5181_IR09.jpg

Slides 18bina_Presentation_IR09_Jehin.pdf

Video 18bina_Presentation_IR09_Jehin.mp4

10:10 → 11:10 3. Data & Science with other telescopes of interest

10:10 Galactic sources at low radio frequency

We have started a programme with Giant Metrewave Radio Telescope (GMRT) to survey the Cygnus OB2 region at 325 and 610 MHz. The Cygnus OB2 region is rich with a wide variety of sources across the electromagnetic spectrum such as protostars, young massive stars, X-ray sources, unidentified VHE sources, colliding wind binaries, shells, bubbles, shocks, etc. Frequencies below 1 GHz trace the non-thermal emission and GMRT offers good resolution and sensitivity at these frequencies. This survey, in combination with available multi-wavelength data, will help us to characterise thermal - non-thermal emission in galactic radio sources.

Speaker: Prof. Anandmayee Tej (Indian Institute of Space Science and Technology, Thiruvananthapuram, India)

Pictures 18bina_Picture_DSC5189_IR10.jpg

Slides 18bina_Presentation_IR10_Chenakkod.pdf

Video 18bina_Presentation_IR10_Chenakkod.mp4

10:50 Application of Convolutional Neural Networks for Stellar Spectral Classification

We propose an automated approach for the classification of stellar spectra using Deep Neural Networks. Due to the ever-expanding volume of observed spectroscopic data from surveys such as SDSS and LAMOST, it has become important to apply artificial intelligence (AI) techniques for analysing stellar spectra to solve spectral classification and regression problems like the determination of stellar atmospheric parameters Teff, log g and [Fe/H]. Traditional machine learning methods with "shallow" architecture (usually up to 2 hidden layers) have been trained for these purposes in the past. However, deep learning methods with a larger number of hidden layers allow the use of finer details in the spectrum which results in improved accuracy and better generalisation. Studying finer spectral signatures also enables us to find rare objects and outliers. Moreover, such models trained on empirical libraries provide wider coverage of the parameters space as compared to synthetic libraries. We examine various machine and deep learning algorithms like Artificial Neural Networks (ANN), Convolutional Neural Networks (CNN), and Autoencoders to classify stellar spectra using the Jacoby Atlas, and ELODIE and MILES spectral libraries as training samples. We test the performance of the trained networks on the Indo-U.S. Library of Coudé Feed Stellar Spectra (CFLIB). We show that using autoencoders, we are able to achieve a precision of 1.5 spectral sub-classes in the classification scheme as compared to the precision of up to 2 sub-classes achieved in the past studies. The trained model can further be used to classify stellar spectra from large databases (e.g SDSS) with better precision and could also be implemented in data-analysis pipelines for various survey programs. With the latest GAIA release, we also plan to take advantage of distances from this mission to compile a better training sample.

Speaker: Dr Kaushal Sharma (Inter University Centre for Astronomy and Astrophysics)

Slides 18bina_Presentation_CT16_Sharma.pdf

Video 18bina_Presentation_CT16_Sharma.mp4

11:10 → 11:30 Coffee/Tea break

11:30 → 12:50 3. Data & Science with other telescopes of interest: 2. Galactic astronomy with other telescopes of interest

11:30 Evolution of magnetic activities on active solar-type stars: starspot modulation, surface differential rotation, and flares

Solar-type stars with a similar internal structure to that of the Sun (spectral type from late-F to early-M) are supposed to operate a similar type of dynamo mechanism. However, the observations of these stars have introduced a range of stellar rotation periods, gravities, masses, and ages, which put into the debate on the existing magnetic dynamo theory. In order to provide useful constraints for the dynamo theory, we are currently working on a project to investigate the magnetic activities of the stars with the same internal structure. We have chosen the F-type star KIC6791060, the K-type star LO Pegasi, and M-type planet-hosting stars EPIC211901114 and K2-33. We intend to compare the results with those of the Sun. Using several ground-based (mostly from BINA telescopes) and space-based observatories, we intend to study the photospheric, upper chromospheric and coronal activity indicators. Using ~24 years long multi-band photometric data, we derive the rotational period of LO Peg to be 0.4231 ± 0.0001 d. Using the seasonal variations on the rotational period, the surface differential rotation (SDR) pattern is investigated and shows a solar-like pattern of SDR with a period of ∼2.7 yr. A total of 20 optical flares are detected with a flare frequency of ∼1 flare per two days and a flare energy of ∼10^{31–34} erg. The surface coverage of cool spots is found to be in the range of ∼9–26%. A flip-flop cycle of ~1 yr appears to be present. Using 4 years long multi-band observations of KIC6791060 and three months observations of EPIC211901114 and K2-33 along with the observations with ground-based observatories, we have recreated the surface inhomogeneity map. We also analysed for habitability on those orbiting planets.

Speaker: Dr Subhajeet Karmakar (Aryabhatta Research Institute of Observational Sciences (ARIES))

Video 18bina_Presentation_CT17_Karmakar.mp4

11:50 Three years of AstroSat: India's first mission dedicated to astronomy

AstroSat, India’s first dedicated astronomy mission has successfully completed its third year in orbit. The AstroSat observatory carries five astronomy payloads covering from ultraviolet to soft/medium energies to hard X-rays. The data from AstroSat has led to several new scientific results like X-ray polarisation using the Cadmium Zinc Telluride Imager (CZTI) and solving of a twenty years puzzle of a cool red star in NGC 188 which is simultaneously very bright in ultraviolet too with the help of the UltraViolet Imaging Telescopes (UVIT). In addition we have detected beat period in X-rays in a magnetic cataclysmic variable V2400 Oph which makes it a discless intermediate polar. This makes it an unique cataclysmic variable as intermediate polars with their low magnetic fields do not disrupt the accretion disc. I will be summarising this detection and will discuss other exciting results from AstroSat in general.

Speaker: Girish V (ISRO)

Pictures 18bina_Picture_DSC5197_CT18.jpg

Slides 18bina_Presentation_CT18_Veerappa.pdf

Video 18bina_Presentation_CT18_Veerappa.mp4

12:10 The ultraviolet imaging telescope on-board AstroSat: recent results

The UltraViolet Imaging Telescope (UVIT) is one of the scientific payloads on board India's first multi-wavelength astronomical satellite AstroSat launched by the Indian Space Research Organisation on 28 September 2015. Along with UVIT and other X-ray instruments, AstroSat has the unique capability of simultaneously imaging a celestial source from the ultraviolet to the hard X-ray band. UVIT is working as per the design specifications and has started to produce interesting results. This talk will focus on details of UVIT, its unique capabilities, planning an observation with UVIT, recent interesting results from UVIT and possible synergies between UVIT and other Belgian telescopes.

Speaker: Dr Stalin Chelliah Subramonian (Indian Institute of Astrophysics, Bangalore)

Pictures 18bina_Picture_DSC5201_CT19.jpg 18bina_Picture_DSC5202_CT19.jpg

12:30 Spectroscopic view on the pulsating A-type stars HD 73045 and HD 118660

This talk reviews the results of a spectroscopic study of two pulsating A-stars. HD 118660 was known as a photometric variable star whose physical properties had been studied with the use of spectroscopy from the Russian 6-m Большой Телескоп Альт-азимутальный (BTA). Here, we present the direct spectroscopic confirmation of the pulsational nature of the star and outline the requirements for the further study. HD 73045 is a spectroscopic binary SB1-type star with a pulsating component. This star had been extensively observed with the Main Stellar Spectrograph of the BTA in March 2015. That monitoring revealed the changes of radial velocity with a period close to four hours. In this study we have re-analysed the data from the Special Astrophysical Observatory (SAO) and compare them with the results of spectroscopic monitoring carried out with the HERMES spectrograph from the Roque de los Muchachos Observatory (RMO) in La Palma, Spain.

Speaker: Dr Eugene Semenko (Special Astrophysical Observatory, Nizhnii Arkhyz, Russia)

Pictures 18bina_Picture_DSC5204_CT20.jpg

Slides 18bina_Presentation_CT20_Semenko.pdf

12:50 → 13:10 Workshop picture

13:10 → 14:30 Lunch break

14:30 → 19:30 Social events

19:30 → 22:30 Workshop dinner

22:30 → 23:00 End of day 3

Friday, 12 October

09:00 → 09:30 Start of day 4 (Meridian room opens)

09:30 → 11:10 3. Data & Science with other telescopes of interest: 2. Galactic astronomy with other telescopes of interest

09:30 Stellar and galactic studies with the 2-m Himalayan Chandra Telescope

The Himalayan Chandra Telescope (HCT), Indian Astronomical Observatory (IAO), Hanle, India, has entered its 15th year of operation. Over the years, various observational programs have been carried out leading to a large number of publications. A brief overview of stellar and galactic studies carried out using HCT and its back end instruments such as the Himalaya Faint Object Spectrograph (HFOSC) and Hanle Echelle Spectrograph (HESP) will be presented. Some important science results will be highlighted with the aim to expand potential collaboration in the area of stellar and galactic studies using these observing facilities.

Speaker: Prof. Aruna Goswami (Indian Institute of Astrophysics, Bangalore)

Pictures 18bina_Picture_DSC5264_CT21.jpg 18bina_Picture_DSC5265_CT21.jpg

09:50 Spectroscopic studies of carbon-enhanced metal-poor stars

The halo system of the Milky Way comprises the vast majority of the presently observed metal-poor ([Fe/H]< -1.0) and very metal-poor ([Fe/H] < -2.0) stars. Among these metal-poor stars, a sizable fraction (~30%) show carbon enhancement ([C/Fe] > 1.0). These stars are called Carbon-Enhanced Metal-Poor (CEMP) stars. Studies of these objects are of special interest, since they bear the fossil records of nucleosynthesis of the first generation of stars and thus provide insight into the nucleosynthesis and chemical evolution of the early universe. In the recent past, although these stars have drawn considerable attention as far as their spectroscopic studies are concerned, several questions still remain poorly understood such as the origin and the production mechanism(s) of carbon and neutron-capture elements exhibited by these objects. A comprehensive study of the abundance patterns of various heavy elements in these objects can give important clues to these questions. We have undertaken to perform chemical composition studies of a selected sample of CEMP stars using the 2-m HCT/HESP and ESO-MPI/FEROS. The abundance distribution patterns and the elemental abundance ratios are critically examined to understand their origin and evolution. We will present some results obtained from our recent spectroscopic studies. Such studies can be highly enhanced through BINA collaborations involving many institutes.

Speaker: Prof. Aruna Goswami (Associate professor)

10:10 Probing the Galactic s-process nucleosynthesis using metal-deficient Barium stars

The origin and evolution of neutron-capture elements in our Galaxy is poorly understood. Detailed chemical composition analysis of stars with the atmosphere enriched by these elements can throw light on the Galactic chemical evolution history. Metal-deficient Ba stars form useful candidates for this kind of studies. They are mostly in their main-sequence and giant phase of stellar evolution with enhanced abundance of neutron-capture elements in their surface. Nucleosynthesis theories do not support the occurrence of s-process nucleosynthesis during the stellar evolutionary phases to which these stars belong. Low and intermediate mass stars in their Asymptotic Giant Branch (AGB) phase are known to produce the s-process elements. Most of the barium stars are known to be binary systems and they are believed to have received via binary mass transfer mechanisms the products of the companion stars produced during their AGB phase of evolution. Hence, the chemical composition of this class of objects can be used to trace back the AGB nucleosynthesis at their corresponding metallicities. The [hs/ls] ratio (hs/ls refer to the heavy/light s-process elements, respectively) could give clues to the accurate origin of the s-process nucleosynthesis, the reactions operating at different metallicities. The C/O ratio and 12C/13C ratio can provide insight into the evolutionary status of the star and different nucleosynthesis and mixing processes happening in the stellar interiors, while the [Rb/Sr] ratio provides the mass of AGB star. We will present the results of detailed spectroscopic study of a selected sample of Ba stars performed along this line based on the high-resolution optical spectroscopic observations using 2-m HCT/HESP, 8.2-m VLT/UVES and ESO-MPI/FEROS. Possibilities of taking forward such studies in the framework of BINA collaboration will be discussed.

Speaker: Ms Shejeelammal J (Student)

Pictures 18bina_Picture_DSC5270_CT23.jpg

Slides 18bina_Presentation_CT23_Jameela.pdf

Video 18bina_Presentation_CT23_Jameela.mp4

10:30 Probing high-mass star-formation in the outflow source G12.42+0.50

The formation of high-mass stars remains an enigmatic process. Through a multi-wavelength study of G12.42+0.50, designated as an outflow source, we probe the various associated components that shed crucial light on the processes involved in the early phases of massive star formation. We present the first low-frequency radio observations of this source and attempt to reveal the nature of this source and the radiation mechanism responsible for the radio emission. Near-infrared spectroscopy is carried out to identify the spectral carriers responsible for the enhanced 4.5 micron emission seen. Further, gas kinematics from molecular line data is investigated to build an overall star formation scenario associated with G12.42+0.50.

Speaker: Prof. Anandmayee Tej (Indian Institute of Space Science and Technology, Thiruvananthapuram, India)

Slides 18bina_Presentation_CT24_Tej.pdf

Video 18bina_Presentation_CT24_Tej.mp4

10:50 High-mass star formation toward the southern infrared bubble S10

An investigation in radio and infrared wavelengths of two high-mass star-forming regions toward the southern Galactic bubble S10 is presented in this work. The two regions under study are associated with the broken bubble S10 and Extended Green Object, G345.99-0.02, respectively. Radio continuum emission mapped at 610 and 1280 MHz using the Giant Metrewave Radio Telescope, India, is detected toward both of the regions. These regions are estimated to be ionized by early-B- to late-O-type stars. Spitzer GLIMPSE mid-infrared data is used to identify young stellar objects (YSOs) associated with these regions. A Class-I/II-type source, with an estimated mass of 6.2 Msun, lies ~7′′ from the radio peak. Pixel-wise, modified blackbody fits to the thermal dust emission using Herschel far-infrared data is performed to construct dust temperature and column density maps. Eight clumps are detected in the two regions using the 250 μm image. The masses and linear diameter of these range between ~300–1600 Msun and 0.2–1.1 pc, respectively, which qualifies them as high-mass star-forming clumps. Modeling of the spectral energy distribution of these clumps indicates the presence of high luminosity, high accretion rate, massive YSOs possibly in the accelerating accretion phase. Furthermore, based on the radio and mid-infrared morphology, the occurrence of a possible bow wave toward the likely ionizing star is explored.

Speaker: Prof. Anandmayee Tej (Indian Institute of Space Science and Technology, Thiruvananthapuram, India)

Slides 18bina_Presentation_CT25_Das.pdf

Video 18bina_Presentation_CT25_Das.mp4

11:10 → 11:30 Coffee/Tea break

11:30 → 13:10 3. Data & Science with other telescopes of interest: 3. Extragalactic astronomy with other telescopes of interest

11:30 Optical and X-ray observations of three candidate polars: RX J0859.1+0537, RX J0749.1-0549, and RX J0649.8-0737

We present analyses of optical (photometric and spectroscopic) data obtained from 1-m class telescopes at ARIES (Nainital) and the 2.01-m Himalayan Chandra Telescope (HCT) at Indian Astronomical Observatory (IAO), Hanle, India, for three candidate polars namely RX J0859.1+0537, RX J0749.1-0549, and RX J0649-0737. An analysis of X-ray data obtained from the ROSAT satellite is also presented. Optical photometric and X-ray observations of these three candidates reveal eclipse features that are deep, total, and variable in shape and are classified for the first time as eclipsing polars. The optical and X-ray modulations of RX J0859.1+0537, RX J0749.1-0549, and RX J0649.8-0737 are found to occur at the derived orbital periods of 2.390 +/-0.003, 3.67 +/- 0.001, and 4.340 +/- 0.001 hr, respectively. Among these systems, RX J0859.1+0537 is found to be the 12th eclipsing polar which lies in the period gap, while RX J0749.1-0549 and RX J0649.8-0737 are found to be the 6th and 7th long period eclipsing polars. The eclipse width at half depth was observed to be more than ∼0.2 for each system which suggests that these are highly inclined binary systems. The optical spectra of these systems are typical of polars with strong high ionization emission lines and inverted Balmer decrement which further confirms the magnetic nature of these systems.

Speaker: Ms ARTI JOSHI (Aryabhatta Research Institute of observational sciencES (ARIES))

11:50 Ground-based photometric survey to search for the pulsational variability in Ap and Am Stars

A survey project called the “Nainital-Cape Survey” was started in the late 1990s with the aim to search and study pulsation in Ap & Am stars using the observing facilities from Nainital and Cape Town. This ongoing survey programme has monitored so far more than 350 stars and has discovered pulsation variability in one roAp and seven Delta Scuti stars. Recently, we obtained time-series PMT observations of five new Ap stars from the 0.5-m telescope at the South African Astronomical Observatory. Analysis of our data shows that none of the these sample exhibit photometric variability, hence classified as null results. The follow-up time-series CCD photometric observations of two Delta Scuti stars, namely, HD13038 and HD13079 were carried out from 1.04-m and 1.3-m telescope of the Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital. The differential photometry of the star HD13038 gives a strong evidence of a new periodicity of 84.98 min. Similarly, in HD13079, we found the pulsation period of 73.8 min and 72.9 min on two different nights. Those are almost consistent to the previously reported values. In this talk, I will give a brief summary of the present status of the Nainital-Cape survey project along with the current activities.

Speaker: Dr Santosh Joshi (ARIES, Nainital)

Pictures 18bina_Picture_DSC5291_CT27.jpg

Slides 18bina_Presentation_CT27_JoshiS.pdf

Video 18bina_Presentation_CT27_JoshiS.mp4

12:10 The spectroscopic survey of southern oEA stars

I will give a review on pulsation properties of the group of mass-accreting components of Algols (oEA stars). I will discuss the importance of detection of high-degree nonradial pulsations (NRP). The precise monitoring of frequencies of high-degree NRPs allows tracking the micro-variations (acceleration and braking) of the surface layers of oEA stars under high mass-transfer events. I will report about first results of the ongoing high-resolution spectroscopic survey of oEA stars started in 2017 using the SALT telescope and aimed to detect the high-degree NRP in Southern oEA stars.

Speaker: Dr David Mkrtichian (NARIT)

Pictures 18bina_Picture_DSC5301_CT28.jpg

12:30 Prospects for radio observations of Particle-Accelerating Colliding-Wind Binaries with the Giant Metrewave Radio Telescope

Synchrotron radiation identified in the radio domain for several tens of binary systems made of massive stars provides compelling evidence that a particle acceleration process is at work in these objects, hence their Particle-Accelerating Colliding-Wind Binaries (PACWB) status. Measurements of the synchrotron radio emission allow to investigate the non-thermal physics and to derive some of their properties. In this context, it is worth investigating the expectations from longer wavelengths such as those measured by the Giant Metrewave Radio Telescope (GMRT) in India, in complementarity with the most abundant measurements at centimetric wavelengths obtained with other radio observatories such as the Very Large Array (VLA) or the Australia Telescope Compact Array (ATCA). This talk will outline such expectations and address the issue of the underlying physics in its appropriate context.

Speaker: Dr Michaël De Becker (STAR, Liège University)

Pictures 18bina_Picture_DSC5304_CT29.jpg

Slides 18bina_Presentation_CT29_DeBecker.pdf

Video 18bina_Presentation_CT29_DeBecker.mp4

12:50 Understanding physical properties of M-dwarfs: near-infrared (HK band) spectroscopic studies

A sample of young M-dwarfs from young moving groups and old population from the galactic field is observed using the near-infrared TIRSPEC instrument (R=1200) on the 2-m Himalayan Chandra Telescope (HCT) at Hanle. Using interferometrically measured effective temperatures, radii, luminosities of a sample of calibrators with spectral type ranging from M0 V to M6 V, we have developed modified empirical calibration relations based on HK-band TIRSPEC spectra. The standard deviations in the residuals of our best fits for Teff and radii are 100 K and 0.03 Rsun, respectively. The metallicities [Fe/H] and [M/H] of M-dwarfs are estimated from Na I, Ca I equivalent widths and H2O - K2 index. The characterization of M-dwarfs is important to future exoplanet missions targeting for potential habitable exoplanet host stars.

Speaker: Dr Soumen Mondal (S. N. Bose National Centre for Basic Sciences)

Video 18bina_Presentation_CT30_Khata.mp4

13:10 → 14:30 Lunch break

14:30 → 15:50 3. Data & Science with other telescopes of interest: 3. Extragalactic astronomy with other telescopes of interest

14:30 Multi-wavelength extragalactic astronomy

Galaxies are generally considered as the basic building blocks of the Universe. Besides stars, galaxies also contain a multi-phase interstellar medium that consists of molecules, atoms, ions, and dust grains. A global picture of the structure, formation, and evolution of galaxies requires observations of all these different components, and hence a multi-wavelength approach. We will describe some recent advancements of our understanding of nearby galaxies, based on multi-wavelength data from ultraviolet to radio wavelengths, combined with state-of-the-art numerical modelling.

Speaker: Prof. Maarten Baes (Universiteit Gent)

Pictures 18bina_Picture_DSC5325_IR11.jpg

Slides 18bina_Presentation_IR11_Baes.pdf

Video 18bina_Presentation_IR11_Baes.mp4

15:10 DustKING - the story continues: dust attenuation in NGC628

Dust attenuation is a crucial but highly uncertain parameter that hampers the determination of intrinsic galaxy properties, such as stellar masses, star formation rates and star formation histories. The shape of the dust attenuation law is not expected to be uniform between galaxies, nor within a galaxy. Our DustKING project was introduced at the first BINA workshop in 2016 and studies the variations of dust attenuation curves in nearby galaxies. To this aim, we used the CIGALE code to fit the observed spectral energy distribution. Particularly important for our goal are ultraviolet (UV) data from the SWIFT space telescope, whose filters cover the curious bump feature in the attenuation curve at 2175 Å. As a follow-up of the previous talk, I will present the final results for the spiral galaxy NGC628 (Decleir et al., to be submitted soon). We found that the average attenuation law of this galaxy is characterised by a MW-like bump and a very steep slope. Also, there are some interesting correlations between dust attenuation properties and other galaxy properties. Finally, we showed that UV data are inevitable for our study. Therefore, we would like to use the UVIT from the Indian AstroSat mission in the future. My talk will focus on the possibilities of using this instrument and propose a possible collaboration within the BINA framework.

Speaker: Ms Marjorie Decleir (Universiteit Gent)

Pictures 18bina_Picture_DSC5328_CT31.jpg

Slides 18bina_Presentation_CT31_Decleir.pdf

Video 18bina_Presentation_CT31_Decleir.mp4

15:30 Multi-wavelength variability and quasi-periodic oscillations in blazars

Blazar is a sub-class of radio loud active galactic nuclei (AGN). Blazars show large amplitude flux and polarization variability in the complete electromagnetic spectrum and emission being pre-dominantly nonthermal. Occasionally quasi-periodic oscillations (QPOs) are also reported in blazars time series data. In the talk, I will discuss about our recent results obtained using multi-wavelength observational facilities around the globe.

Speaker: Dr Alok Chandra Gupta (ARIES, Nainital, India)

Slides 18bina_Presentation_CT32_Gupta.pdf

15:50 → 16:10 Coffee/Tea break

16:10 → 16:50 4. Workshop summary

slides 18bina_Presentation_IR12_Prugniel.pdf

16:50 → 17:00 Closing ceremony

Pictures 18bina_Picture_DSC5363_CS04.jpg

17:00 → 17:30 End of day 4 (Meridian room closes)