### An Occultation Network as a Detector of Distant Solar System Objects

We discuss the feasibility of and present initial designs and cost estimates for a large (N~2000) network of small photometric telescopes that is purpose-built to monitor V15 Gaia Mission program stars for occultations by minor solar system bodies. The implementation of this network would permit measurement of the solar system's tidal gravity field to high precision, thereby revealing the existence of distant trans-Neptunian objects such as the proposed “Planet Nine". As a detailed example of...

### The APPLAUSE-Projekt: The plate archives

The Dr. Remeis-Sternwarte in Bamberg, the Leibniz-Institut für Astrophysik, Potsdam and the Hamburger Sternwarte host important astronomical plate archives. Astronomers from those institutions teamed up to digitize their archives, calibrate and integrate them into the publically available database APPLAUSE. In an international collaboration also the plate archive of the Tartu observatory was included. Here we briefly describe the instrumentations used and the history of the plate archives of the collaboration.

### Observatorium Wendelstein – Status, Use and Future Strategy

We will describe the capabilities of the Observatorium Wendelstein (University of Munich,LMU), mainly of its 2m telescope with its three operational imaging and spectroscopic instruments. We will describe their performances based on a few science examples, partly survey type programs. Finally, we will discuss strategies how to benefit from the Wendelstein Observatory in times of up-coming new major astronomy resources.

### Astronomical Photographic Archives: Past, Present, Future

There are more than 10 millions astronomical photographic negatives (glass plates and planfils/films) worldwide. Most of them represent stellar fields and solar images, but there are also numerous negatives with other celestial objects. There is large variety of these negatives (wide field and narrow field direct images, multiple images, low dispersion and high dispersion spectra etc.). I will give review and discussion of these databases including recent progress in their digitization and scienfic use.

### Sternberg Astronomical Institute’s plate collection: the present and future of its scientific use

There are more than 10 millions astronomical photographic negatives (glass plates and planfils/films) worldwide. Most of them represent stellar fields and solar images, but there are also numerous negatives with other celestial objects. There is large variety of these negatives (wide field and narrow field direct images, multiple images, low dispersion and high dispersion spectra etc.). I will give review and discussion of these databases including recent progress in their digitization and scienfic use.Direct plates...

### Large Surveys with Small Telecsopes: Abstracts of the Conference Talks and Posters

The booklet contains the submitted abstracts for the conference. Some contributions were not presented in the conference, others were late additions. Each presented contribution, where the authors submitted their slides or poster have been given a separate DOI.

### Gaia: Second Data Release

Gaia Data Processing, Friedrich Anders, Christina Chiappini & Arman Khalatyan
Estimating Distance from Parallaxes. Distances to 1.33 Billion Stars in Gaia Data Release 2. For the vast majority of stars in the second Gaia data release, reliable distances cannot be obtained by inverting the parallax. A correct inference procedure must instead be used to account for the nonlinearity of the transformation and the asymmetry of the resulting probability distribution. Here, we infer distances to essentially all 1.33 billion stars with parallaxes published in the second...

### The Gaia catalogue of hot subluminous stars

Based on data from the ESA Gaia Data Release 2 (DR2) and several ground-based, multi-band photometry surveys we have compiled an all-sky catalogue of 39800 hot subluminous star candidates selected in Gaia DR2 by means of colour, absolute magnitude, and reduced proper motion cuts. We expect the majority of the candidates to be hot subdwarf stars of spectral type B and O, followed by blue horizontal branch stars of late B-type (HBB), hot post-AGB stars,...

### Astronomical plates digitization by digital camera

Digitization by transportable device based on digital camera represents alternative technique for astronomical plate archives digitization worldwide. Several plate collections were digitized this way, e.g. Tuorla, Mexico, and Hewitt UK. Digitization of astronomical plate archives in Austria is planned for 2019. The technique is very fast, hence inexpensive, still providing scientific grade accuracy.

### Hamburg Quasar Survey

The Hamburg Quasar Survey carried out 1985 - 1997 was using the Calar Alto Schmidt telescope equipped with an objective prism. The survey covered the Northern sky at galactic latitudes b > 20 deg, and declination delta > 0 deg). The spectroscopic Schmidt contain usable spectra with a seeing limited resolution of 45 Angstroem at Hgamma in the magnitude range 14 < B < 19. The HQS archive contains 1288 plates for 567 fields. These...

### The LAMOST II medium-resolution survey

LAMOST survey is a Chinese-operated spectroscopic survey using a 4-meter reflective Schimdt telescope. Since 2011, it has collected about 10 million low-resolution spectra, most of which are stellar spectra. The LAMOST survey continuously covering a large fraction of northen sky allows for broad studies about the Milky Way, especially for the Galactic outer disk. I will briefly highlight the achievment of the LAMOST survey in stellar physics and the Milky Way science. Then I will...

### The RAVE survey - Final Data Release

Results of the RAVE Survey

### Showing the possibility of N(ear)R(eal)T(ime) creation of WCS solutions with solvefield for a complete sky survey

W. Fürtig M. Ennes
The detection of fast moving or new objects on sky surveys with small cameras depend largely on the creation of a valid WCS solution for each image. A short time for detecting these objects on images is crucial for subsequent time critical actions to be taken. For comparing found sources with online catalogs a valid WCS is neeeded. The more time spent for getting an initial or iterative wcs solution the less time for other...

### SPECULOOS - On the hunt for habitable planets well-suited for atmospheric characterization

After the astonishing discovery of seven Earth-sized planets around TRAPPIST-1, a Jupiter-sized star only 12 pc away, the hunt for temperate, rocky exoplanets goes into its next phase. The SPECULOOS survey is a new transit survey focusing on the ~1000 brightest (K$\leq$12.5) ultra-cool dwarfs (spectral type M7 or later). Its main objective is to detect temperate terrestrial worlds well-suited for detailed atmospheric characterization with upcoming JWST and ELTs. It also aims to probe the frequency...

### Newest results of the Next Generation Transit Survey (NGTS)

In 2018 the firsts transiting exoplanets discovered with NGTS have been published. NGTS consists of twelve telescopes sited at ESO premise on Paranal, Chile. The optimal photometric conditions on site combined with the optimized instrument allow us to detect signals a magnitude smaller compared to previous ground based wide field surveys. With the sensitivity reaching more into the red wavelength NGTS focus to detect Neptune sized planets around K-dwarfs. One of these planets is NGTS-4b...

### False-positives detection with convolutional neural networks

Digital scans of photographic plates are more complicated to handle in comparison to the CCD frames. Due to their fragile nature and age they are subject to several effects that act as a source of false-positive detections. Among these effects are surface dust speckles, scratches, emulsion damage, and writing traces. Besides those the optical systems used to acquire the images come with their share of aberrations which make the removal of false-positives harder. The APPLAUSE...

### PLATO deep-field south: its input catalog from BMK10k observations

PLATO is ESA’s M3 mission for launch in 2026. It will search for extrasolar planets by means of ultra-high-precision transit photometry. This requires a well-selected and well-defined stellar input sample for optimized planet harvesting. Two long-duration PLATO fields form the core of the mission. The one field in the southern hemisphere will be observed with BMK10k well in advance of the mission for support of its target input catalog.The BMK10k survey will provide well-sampled light...

### Pulsating stars with TESS

The Transiting Exoplanet Survey Satellite (TESS; Ricker et al., 2015, JATIS 1, 014003) was launched on April 18, 2018, and started its scientific observations on June 25, 2018. It is gathering ultra-precise photometric observations for celestial objects with I_C $\approx$ 4 – 13 and an ecliptic latitude above 6 degrees. Preselected targets are observed with a cadence of 2 minutes while full-frame images are obtained every 30 minutes. In two years time, the largest part...

### Records from the past: variable stars from the Asiago plate archive

Direct plates archives may be used to remeasure stars which were the target of the observations or to look at other stars discovered to be interesting only at a later time. I present here two cases: a search for Long Period Variable (LPV) stars on IR plates, and a search for past outbursts of a recently discovered cataclismic variable.Long period red variables (LPV) have been searched in a collection of Schmidt plates of the Asiago...

### Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18

Friedrich Anders, Christina Chiappini & Arman Khalatyan
Estimating Distance from Parallaxes. Distances to 1.33 Billion Stars in Gaia Data Release 2. For the vast majority of stars in the second Gaia data release, reliable distances cannot be obtained by inverting the parallax. A correct inference procedure must instead be used to account for the nonlinearity of the transformation and the asymmetry of the resulting probability distribution. Here, we infer distances to essentially all 1.33 billion stars with parallaxes published in the second...

### Lippert-Astrograph (Hamburg), Envelope 14304

Lippert-Astrograph (Hamburg), Envelope : 14304

### Bamberg Southern Sky Patrol (New Zealand), Envelope 63266

Bamberg Southern Sky Patrol (New Zealand), Envelope : 63266

### Impact of the ASAS-SN survey and the Moscow's photographic plates archive on the nature of the emission line star HBHA 1704-05

The star HBHA 1704-05 was originally classified as an emission-line star (Kohoutek and Wehmeyer, 1999). On the basis of The All Sky Automated Survey for SuperNovae (ASAS-SN), the object was cataloged in the VSX as an semi-regular variable with a periodicity around 418 days. At the beginning of August 2018, the ASAS-SN survey indicated a rapid brightening of the star. Following high-cadence photometric and spectroscopic observations clarified the nature of HBHA 1704-05 as a symbiotic...

### PyPlate: a software package for processing digitized astronomical photographic plates

Digitizing an archive of photographic plates yields a set of image files and accompanying metadata files. To handle and process these data efficiently, we have developed a Python package PyPlate. PyPlate provides methods to read data from CSV and FITS files, to make calculations with various observation timestamps, to create consistent and easily readable FITS headers, to write plate metadata into a database, to extract sources from plate images, to carry out astrometric and photometric...

### Surveying exoplanets across the spectrum - following the TraCS of exoplanets

In this talk, I will describe the efforts done by the Wendelstein observatory in following up known exoplanets and planet candidates both spectroscopically and photometrically. We are currently installing a high-resolution spectrograph, calibrated with an LFC, and a simultaneous 3-channel camera that covers photometric bands between u and Ks. With the latter, we are currently performing a transit survey where we observe primary and secondary in order to determine their Transit Colour Signature (TraCS).

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