scholarly journals A search for transiting planets in the Galactic Plane

2008 ◽  
Vol 4 (S253) ◽  
pp. 343-345
Author(s):  
Veronica R. Miller ◽  
Michael D. Albrow
Keyword(s):  
Extrasolar Planets ◽  
Galactic Plane ◽  
Wide Field ◽  
Transiting Planets ◽  
Deep Survey ◽  
Initial Results

AbstractWe are carrying out a deep survey for transiting extrasolar planets in a 1 square degree field in the Galactic Plane. The images to date were taken using the Wide Field Imager on the ESO 2.2m telescope at La Silla. We present details of the analysis and initial results from the survey.

scholarly journals Search for Transiting Exoplanets with HATNet

2008 ◽  
Vol 4 (S253) ◽  
pp. 21-27
Author(s):  
G. Á. Bakos ◽  
R. W. Noyes ◽  
G. Kovács ◽  
D. W. Latham ◽  
G. Torres ◽  
...  
Keyword(s):  
High Resolution ◽  
Extrasolar Planets ◽  
Detection Efficiency ◽  
False Alarms ◽  
Wide Field ◽  
Transiting Planets

AbstractHATNet is a network of six identical, fully automated wide field telescopes, four of which are located in Arizona, and two at Hawaii. The purpose of the network is to search for transiting extrasolar planets around relatively bright stars (8 <I< 12). The longitudinal coverage of 3.5 hours greatly enhances transit detection efficiency. HATNet has been operational since 2004, and has taken more than 1/2 million science frames at 5-min integrations, covering about 7% of the sky. Photometric precision reaches 3mmag rms at 5.5 min cadence atI≈ 8, and is 1% atI≈ 11.3. Hundreds of transitcandidateshave been detected in the data, and have been subject to vigorous follow-up by various 1m-class facilities, both spectroscopy and follow-up photometry. A fraction of the candidates that have survived these steps as not being false alarms have been observed by high resolution and precision spectrographs (primarily Keck/HIRES), to confirm their planetary nature and characterize their properties. So far nine transiting planets have been reported, making HATNet a very successful survey.

scholarly journals KELT: A Wide-Field Survey of Bright Stars for Transiting Planets

2008 ◽  
Vol 4 (S253) ◽  
pp. 350-353
Author(s):  
Robert J. Siverd ◽  
Joshua Pepper ◽  
Kris Stanek ◽  
Richard W. Pogge ◽  
B. Scott Gaudi ◽  
...  
Keyword(s):  
Data Reduction ◽  
Field Survey ◽  
Candidate Selection ◽  
Wide Field ◽  
Present Survey ◽  
Transiting Planets ◽  
The Past ◽  
Initial Results ◽  
Sufficient Precision

AbstractThe Kilodegree Extremely Little Telescope (KELT) is a wide-field (26° × 26°) robotic survey telescope currently operating in Sonoita, Arizona. Assembled from commercial and off-the-shelf devices, KELT currently surveys ~40% of the Northern sky with sufficient precision to detect transiting planets around bright (8 < V < 12) stars. In the past several years of operation, over 30,000 science images have been acquired. Planet candidate selection and follow-up are currently underway. A brief overview of past and present survey operations, the data reduction pipeline, and initial results follows below.

The Hubble Space Telescope Medium Deep Survey with the Wide Field and Planetary Camera. 1: Methodology and results on the field near 3C 273

1994 ◽  
Vol 437 ◽  
pp. 67 ◽  
Author(s):  
R. E. Griffiths ◽  
K. U. Ratnatunga ◽  
L. W. Neuschaefer ◽  
S. Casertano ◽  
M. Im ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Wide Field ◽  
Space Telescope ◽  
Deep Survey

scholarly journals Transit-period search from single-event space-based data: the role of wide-field surveys

2019 ◽  
Vol 625 ◽  
pp. A145
Author(s):  
Geza Kovacs
Keyword(s):  
High Precision ◽  
Wide Field ◽  
Precision Data ◽  
Frequency Spectra ◽  
Transiting Planets ◽  
High Precision Data ◽  
Space Data ◽  
Signal Search

We investigate the optimization of dataset weighting in searching for the orbital period of transiting planets when high-precision space-based data with a single transit event are combined with (relatively) low-precision ground-based (wide-field) data. The optimization stems from the lack of multiple events in the high-precision data and the likely presence of such events in the low-precision data. With noise minimization, we combined two types of frequency spectra: (i) spectra that use two fixed transit parameters (moment of the center of the transit and duration of the event) derived from the space data alone; (ii) spectra that result from the traditional weighted box signal search with optimized transit parameters for each trial period. We used many mock signals to test the detection power of the method. Marginal or no detections in the ground-based data may lead to secure detections in the combined data with the above weighting. Depending on the coverage and quality of the ground-based data, transit depths of ~0.05% and periods up to ~100 days are accessible by the suggested optimum combination of the data.

scholarly journals Extrasolar planet detections with gravitational microlensing

2007 ◽  
Vol 3 (S249) ◽  
pp. 25-30
Author(s):  
Shude Mao ◽  
Eamonn Kerins ◽  
Nicholas J. Rattenbury
Keyword(s):  
Light Curve ◽  
Real Time ◽  
Extrasolar Planets ◽  
Light Curves ◽  
Extrasolar Planet ◽  
Galactic Centre ◽  
Wide Field ◽  
High Magnification ◽  
Gravitational Microlensing

AbstractMicrolensing light curves due to single stars are symmetric and typically last for a month. So far about 4000 microlensing events have been discovered in real-time, the vast majority toward the Galactic centre. The presence of planets around the primary lenses induces deviations in the usual light curve which lasts from hours (for an Earth-mass [M⊕] planet) to days (for a Jupiter-mass [Mj] planet). Currently the survey teams, OGLE and MOA, discover and announce microlensing events in real-time, and follow-up teams (together with the survey teams) monitor selected events intensively (usually with high magnification) in order to identify anomalies caused by planets. So far four extrasolar planets have been discovered using the microlensing technique, with half a dozen new planet candidates identified in 2007 (yet to be published). Future possibilities include a network of wide-field 2m-class telescopes from the ground (which can combine survey and follow-up in the same setup) and a 1m-class survey telescope from space.

scholarly journals The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging

2004 ◽  
Vol 600 (2) ◽  
pp. L93-L98 ◽  
Author(s):  
M. Giavalisco ◽  
H. C. Ferguson ◽  
A. M. Koekemoer ◽  
M. Dickinson ◽  
D. M. Alexander ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Near Infrared Imaging ◽  
Deep Survey ◽  
Initial Results

From BeppoSAX to INTEGRAL: Wide Field Camera results on the Galactic Plane and INTEGRAL prospective

2004 ◽  
Vol 132 ◽  
pp. 580-583 ◽  
Author(s):  
F. Capitanio ◽  
A. Bazzano ◽  
M. Cocchi ◽  
L. Natalucci ◽  
P. Ubertini ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Wide Field

scholarly journals Structure and Mass Function of Open Cluster NGC 6910

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Harmeen Kaur ◽  
Saurabh Sharma ◽  
Alok K. Durgapal
Keyword(s):  
Molecular Clouds ◽  
Luminosity Function ◽  
Open Cluster ◽  
Mass Function ◽  
Open Clusters ◽  
Initial Mass Function ◽  
Wide Field ◽  
Evolutionary Models ◽  
Star Forming ◽  
Initial Results

NGC 6910 is located in a Cygnus X region, which is a ∼10◦ complex of actively star forming molecular clouds and young clusters, located at a distance of about 1.7 kpc (Reipurth & Schneider 2008). Open clusters possess many favorable characteristics for initial mass function (IMF) studies. The observed mass function of a star cluster can in principle be determined from the observed luminosity function (LF) using theoretical stellar evolutionary models. Here, we are presenting our initial results related to structure parameters, extinction, distance and mass function of open cluster NGC 6910 based on the deep and wide field mosaic images taken from 1.0m Sampurnand telescope of ARIES, India.

scholarly journals Structure and Mass Function of Open Cluster NGC 6910

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Harmeen Kaur ◽  
Saurabh Sharma ◽  
Alok K. Durgapal
Keyword(s):  
Molecular Clouds ◽  
Luminosity Function ◽  
Open Cluster ◽  
Mass Function ◽  
Open Clusters ◽  
Initial Mass Function ◽  
Wide Field ◽  
Evolutionary Models ◽  
Star Forming ◽  
Initial Results

NGC 6910 is located in a Cygnus X region, which is a ∼10◦ complex of actively star forming molecular clouds and young clusters, located at a distance of about 1.7 kpc (Reipurth & Schneider 2008). Open clusters possess many favorable characteristics for initial mass function (IMF) studies. The observed mass function of a star cluster can in principle be determined from the observed luminosity function (LF) using theoretical stellar evolutionary models. Here, we are presenting our initial results related to structure parameters, extinction, distance and mass function of open cluster NGC 6910 based on the deep and wide field mosaic images taken from 1.0m Sampurnand telescope of ARIES, India

scholarly journals Mapping large-scale diffuse γ-ray emission in the 10−100 TeV band with Cherenkov telescopes

2020 ◽  
Vol 637 ◽  
pp. A44 ◽  
Author(s):  
A. Neronov ◽  
D. Semikoz
Keyword(s):  
Large Scale ◽  
Galactic Plane ◽  
Cosmic Ray ◽  
Field Of View ◽  
Medium Size ◽  
Wide Field ◽  
Galactic Latitude ◽  
Cherenkov Telescopes ◽  
Diffuse Flux ◽  
Astrophysical Neutrino

Context. Measurement of diffuse γ-ray emission from the Milky Way with Imaging Atmospheric Cherenkov Telescopes (IACT) is difficult because of the high level of charged cosmic ray background and the small field of view. Aims. We show that such a measurement is nevertheless possible in the energy band 10−100 TeV. Methods. The minimal charged particle background for IACTs is achieved by selecting the events to be used for the analyses of the cosmic ray electrons. Tight cuts on the event quality in these event selections allow us to obtain a sufficiently low background level to allow measurement of the diffuse Galactic γ-ray flux above 10 TeV. We calculated the sensitivities of different types of IACT arrays for the Galactic diffuse emission measurements and compared them with the diffuse γ-ray flux from different parts of the sky measured by the Fermi Large Area Telescope below 3 TeV and with the astrophysical neutrino signal measured by IceCube telescope. Results. We show that deep exposure of existing IACT systems is sufficient for detection of the diffuse flux from all the Galactic Plane up to Galactic latitude |b| ∼ 5°. The Medium Size Telescope array of the CTA will be able to detect the diffuse flux up 30° Galactic latitude. Its sensitivity will be sufficient for detection of the γ-ray counterpart of the Galactic component of the IceCube astrophysical neutrino signal above 10 TeV. We also propose that a dedicated IACT system composed of small but wide-field-of-view telescopes could be used to map the 10−100 TeV diffuse γ-ray emission from across the whole sky. Conclusions. Detection and detailed study of diffuse Galactic γ-ray emission in the previously unexplored 10−100 TeV energy range is possible with the IACT technique. This is important for identification of the Galactic component of the astrophysical neutrino signal and for understanding the propagation of cosmic rays in the interstellar medium.

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