Infrared Surveys Planned for ASTRO-F

2005 ◽  
Vol 216 ◽  
pp. 347-352
Author(s):  
Hiroshi Shibai
Keyword(s):  
Far Infrared ◽  
Wide Field ◽  
Wavelength Band ◽  
Mid Infrared ◽  
Field Surveys ◽  
Infrared Wavelength ◽  
Sky Surveys ◽  
Sky Survey ◽  
Infrared Surveys ◽  
Higher Sensitivity

The next survey mission, ASTRO-F, is scheduled for launch in 2005. This is the first Japanese satellite dedicated to infrared astronomy. The primary purpose of this project is to investigate the birth and evolution of galaxies in the early universe through deep, wide-field surveys at wavelengths ranging from 2 to 200 microns. In the far-infrared wavelength band, ASTRO-F will conduct an all-sky survey like the IRAS survey with several tens of times higher sensitivity and several times better spatial resolution. In the near- and mid-infrared, wide area sky-surveys will be conducted over pre-selected portions of the sky in 13 bands ranging from 2-200microns. In addition to these photometric surveys, low-resolution spectroscopic capabilities are available for all wavelength bands. The ASTRO-F mission will produce a fundamental database for the next generation of advanced observatories, for example Herschel, and JWST, and will complement the SIRTF mission by virtue of its wide sky coverage.

scholarly journals The ASTRO-F (IRIS) Mission

2001 ◽  
Vol 204 ◽  
pp. 455-466 ◽  
Author(s):  
Hiroshi Shibai
Keyword(s):  
Spatial Resolution ◽  
Far Infrared ◽  
Wide Field ◽  
Natural Background ◽  
Mid Infrared ◽  
Field Surveys ◽  
Infrared Wavelength ◽  
Sky Survey ◽  
Aperture Diffraction ◽  
Higher Sensitivity

ASTRO-F (IRIS) is the first Japanese satellite dedicated to infrared astronomy. The primary purpose of this project is to investigate the birth and evolution of galaxies in the early universe through deep, wide-field surveys at wavelengths ranging from 2 to 200 microns. The spatial resolution and the point source sensitivity are nearly the same as those of the aperture diffraction limit and the natural background and/or confusion limit, respectively. In the far-infrared wavelength band, ASTRO-F will conduct an all-sky survey like the IRAS survey with several tens of times higher sensitivity and several times better spatial resolution. In the near- and mid-infrared, wide area sky-surveys will be conducted over pre-selected portions of the sky. In addition to these photometric surveys, low-resolution spectroscopic capabilities are available for all wavelength bands. The ASTRO-F mission will produce a fundamental database for the next generation of advanced observatories, for example FIRST, and NGST, and will complement the SIRTF mission by virtue of its wide sky coverage. The launch by an M-V rocket is scheduled for February or March of 2004.

Infrared Wide-Field Surveys

1994 ◽  
Vol 161 ◽  
pp. 13-16
Author(s):  
N. Epchtein
Keyword(s):  
Near Infrared ◽  
Wide Field ◽  
Field Surveys ◽  
Sky Surveys ◽  
The Past ◽  
Infrared Spectral Range ◽  
Sky Survey ◽  
Array Technology ◽  
Infrared Spectral ◽  
Infrared Array

Optical wide-field sky surveys have long been basic tools of astronomical investigations. Their extension to the near infrared spectral range, unattainable with photographic techniques, is now possible thanks to the considerable improvements in infrared array technology that have been achieved in the past few years. The astronomical motivations for all-sky 2 μm surveys are summarized, and a brief technical description of the on-going projects, in particular DENIS (Deep Near Infrared Southern Sky Survey) that will be carried out at the European Southern Observatory in 1994–97, is presented.

scholarly journals YSTAR: Yonsei Survey Telescopes for Astronomical Research

2001 ◽  
Vol 183 ◽  
pp. 83-87
Author(s):  
Yong-Ik Byun ◽  
Won-Yong Han ◽  
Yong-Woo Kang ◽  
Moo-Young Chun ◽  
Sung-Yeol Yu ◽  
...  
Keyword(s):  
South Africa ◽  
Variable Stars ◽  
Primary Objective ◽  
Wide Field ◽  
Target Acquisition ◽  
Data Set ◽  
Field Surveys ◽  
Sky Survey ◽  
Two Factors ◽  
Astronomical Research

AbstractThe YSTAR program is a general sky survey looking for variability. The main equipments are three 0.5-m telescopes. These telescopes have fast F/2 optics covering nearly 3.5 square degree field onto a 2K CCD. They also have very fast slew capability, which exceeds 10 degrees per second. These two factors make them most suitable for rapid target acquisition and wide-field surveys of various kinds. Our primary objective is to identify and monitor variable stars down to 18th R-magnitude, and our observing mode allows the same data set to be also useful in identifying asteroids. Our first telescope has just begun regular automated operation, and the second telescope will be installed in South Africa within this year to provide coverage of the southern sky.

scholarly journals The optical luminosity function of LOFAR radio-selected quasars at 1.4 ≤ z ≤ 5.0 in the NDWFS-Boötes field

2020 ◽  
Vol 636 ◽  
pp. A12
Author(s):  
E. Retana-Montenegro ◽  
H. J. A. Röttgering
Keyword(s):  
Radio Emission ◽  
Luminosity Function ◽  
Field Survey ◽  
Sloan Digital Sky Survey ◽  
Spatial Density ◽  
Spectral Energy ◽  
Wide Field ◽  
Infrared Photometry ◽  
Mid Infrared ◽  
Sky Survey

We present an estimate of the optical luminosity function (OLF) of LOFAR radio-selected quasars (RSQs) at 1.4 <  z <  5.0 in the 9.3 deg2 NOAO Deep Wide-field survey (NDWFS) of the Boötes field. The selection was based on optical and mid-infrared photometry used to train three different machine learning (ML) algorithms (Random forest, SVM, Bootstrap aggregation). Objects taken as quasars by the ML algorithms are required to be detected at ≥5σ significance in deep radio maps to be classified as candidate quasars. The optical imaging came from the Sloan Digital Sky Survey and the Pan-STARRS1 3π survey; mid-infrared photometry was taken from the Spitzer Deep, Wide-Field Survey; and radio data was obtained from deep LOFAR imaging of the NDWFS-Boötes field. The requirement of a 5σ LOFAR detection allowed us to reduce the stellar contamination in our sample by two orders of magnitude. The sample comprises 130 objects, including both photometrically selected candidate quasars (47) and spectroscopically confirmed quasars (83). The spectral energy distributions calculated using deep photometry available for the NDWFS-Boötes field confirm the validity of the photometrically selected quasars using the ML algorithms as robust candidate quasars. The depth of our LOFAR observations allowed us to detect the radio-emission of quasars that would be otherwise classified as radio-quiet. Around 65% of the quasars in the sample are fainter than M1450 = −24.0, a regime where the OLF of quasars selected through their radio emission, has not been investigated in detail. It has been demonstrated that in cases where mid-infrared wedge-based AGN selection is not possible due to a lack of appropriate data, the selection of quasars using ML algorithms trained with optical and infrared photometry in combination with LOFAR data provides an excellent approach for obtaining samples of quasars. The OLF of RSQs can be described by pure luminosity evolution at z <  2.4, and a combined luminosity and density evolution at z >  2.4. The faint-end slope, α, becomes steeper with increasing redshift. This trend is consistent with previous studies of faint quasars (M1450 ≤ −22.0). We demonstrate that RSQs show an evolution that is very similar to that exhibited by faint quasars. By comparing the spatial density of RSQs with that of the total (radio-detected plus radio-undetected) faint quasar population at similar redshifts, we find that RSQs may compose up to ∼20% of the whole faint quasar population. This fraction, within uncertainties, is constant with redshift. Finally, we discuss how the compactness of the RSQs radio-morphologies and their steep spectral indices could provide valuable insights into how quasar and radio activity are triggered in these systems.

scholarly journals Search for radio emission from the exoplanets Qatar-1b and WASP-80b near 150 MHz using the giant metrewave radio telescope

2020 ◽  
Vol 500 (1) ◽  
pp. 211-214
Author(s):  
D A Green ◽  
N Madhusudhan
Keyword(s):  
Radio Emission ◽  
Radio Source ◽  
Radio Telescope ◽  
Magnetic Moments ◽  
Wide Field ◽  
Extragalactic Radio Source ◽  
Field Surveys ◽  
Very Large Array ◽  
Sky Survey ◽  
Cross Match

ABSTRACT We present radio observations made towards the exoplanets Qatar-1b and WASP-80b near 150 MHz with the Giant Meterwave Radio Telescope (GMRT). These targets are relatively nearby irradiated giant exoplanets, a hot Jupiter and a hot Saturn, with sizes comparable to Jupiter but different masses and lower densities. Both the targets are expected to host extended H/He envelopes like Jupiter, with comparable or larger magnetic moments. No radio emission was detected from these exoplanets, with 3σ limits of 5.9 and 5.2 mJy for Qatar-1b and WASP-80b, respectively, from these targeted observations. These are considerably deeper limits than those available for exoplanets from wide-field surveys at similar frequencies. We also present archival Very Large Array (VLA) observations of a previously reported radio source close to 61 Vir (which has three exoplanets). The VLA observations resolve the source, which we identify as an extragalactic radio source, i.e. a chance association with 61 Vir. Additionally, we cross-match a recent exoplanet catalogue with the TIFR GMRT Sky Survey ADR1 radio catalogue, but do not find any convincing associations.

OH/IR stars versus YSOs in infrared photometric surveys

2018 ◽  
Vol 14 (S343) ◽  
pp. 454-455
Author(s):  
Cécile Loup ◽  
Mark Allen ◽  
Ariane Lançon ◽  
Anais Oberto
Keyword(s):  
Selection Criteria ◽  
Far Infrared ◽  
High Mass ◽  
Agb Stars ◽  
Infrared Photometry ◽  
Mid Infrared ◽  
Ir Stars ◽  
High Mass Loss ◽  
Infrared Surveys ◽  
Methanol Masers

AbstractAGB stars play a major role in the chemical evolution of the galaxies. It thus is important to establish reliable photometric selection criteria to count them, especially AGB stars at the last stages of AGB evolution like OH/IR stars. Here, we have identified about 1500 OH/IR stars and 500 YSOs with methanol masers, in all major mid– and far–infrared surveys (IRAS, MSX, AKARI, WISE, GLIMPSE, and Hi–Gal). We show that AGB stars with high mass-loss rates cannot be disentagled from YSOs with only mid–infrared photometry; far–infrared photometry is essential. In the region observed by GLIMPSE, we show that the proportion of AGB stars has been severely underestimated in previous works: about 70% of “intrinsically” red objects in GLIMPSE are AGB stars rather than YSOs.

scholarly journals Effectiveness of WISE colour-based selection techniques to uncover obscured AGN

2013 ◽  
Vol 9 (S304) ◽  
pp. 209-212
Author(s):  
S. Mateos
Keyword(s):  
Sloan Digital Sky Survey ◽  
Spectral Energy ◽  
Wide Field ◽  
Mid Infrared ◽  
Selection Technique ◽  
X Ray ◽  
Sky Survey ◽  
Two Samples ◽  
Optical Surveys

AbstractWe present a highly reliable and efficient mid-infrared colour-based selection technique for luminous active galactic nuclei (AGN) using the Wide-field Infrared Survey Explorer (WISE) survey. Our technique is designed to identify objects with red mid-infrared power-law spectral energy distributions. We studied the dependency of our mid-infrared selection on the AGN intrinsic luminosity and the effectiveness of our technique to uncover obscured AGN missed in X-ray surveys. To do so we used two samples of luminous AGN independently selected in hard X-ray and optical surveys. We used the largest catalogue of 887 [OIII] λ5007-selected type 2 quasars (QSO2s) at z≲0.83 in the literature from the Sloan Digital Sky Survey (SDSS), and the 258 hard (>4.5 keV) X-ray-selected AGN from the Bright Ultrahard XMM-Newton Survey (BUXS). The effectiveness of our mid-infrared selection technique increases with the AGN luminosity. At high luminosities and at least up to z~1 our technique is very effective at identifying both Compton-thin and Compton-thick AGN.

scholarly journals The LOFAR Two-metre Sky Survey

2019 ◽  
Vol 622 ◽  
pp. A3 ◽  
Author(s):  
K. J. Duncan ◽  
J. Sabater ◽  
H. J. A. Röttgering ◽  
M. J. Jarvis ◽  
D. J. B. Smith ◽  
...  
Keyword(s):  
Radio Continuum ◽  
Optical Data ◽  
Source Population ◽  
Wide Field ◽  
Radio Luminosity ◽  
Photometric Redshifts ◽  
Mid Infrared ◽  
Strong Trend ◽  
Sky Survey ◽  
Data Release

The LOFAR Two-metre Sky Survey (LoTSS) is a sensitive, high-resolution 120–168 MHz survey of the Northern sky. The LoTSS First Data Release (DR1) presents 424 square degrees of radio continuum observations over the HETDEX Spring Field (10h45m00s < right ascension <  15h30m00s and 45°00′00″ < declination < 57°00′00″) with a median sensitivity of 71 μJy beam−1 and a resolution of 6″. In this paper we present photometric redshifts (photo-z) for 94.4% of optical sources over this region that are detected in the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) 3π steradian survey. Combining the Pan-STARRS optical data with mid-infrared photometry from the Wide-field Infrared Survey Explorer, we estimate photo-zs using a novel hybrid photometric redshift methodology optimised to produce the best possible performance for the diverse sample of radio continuum selected sources. For the radio-continuum detected population, we find an overall scatter in the photo-z of 3.9% and an outlier fraction (|zphot−zspec|/(1 + zspec) > 0.15) of 7.9%. We also find that, at a given redshift, there is no strong trend in photo-z quality as a function of radio luminosity. However there are strong trends as a function of redshift for a given radio luminosity, a result of selection effects in the spectroscopic sample and/or intrinsic evolution within the radio source population. Additionally, for the sample of sources in the LoTSS First Data Release with optical counterparts, we present rest-frame optical and mid-infrared magnitudes based on template fits to the consensus photometric (or spectroscopic when available) redshift.

scholarly journals Performance Estimation of the Mid-Infrared Camera and Spectrometer Aboard SPICA

2015 ◽  
Vol 04 (01n02) ◽  
pp. 1550001 ◽  
Author(s):  
Hirokazu Kataza ◽  
Itsuki Sakon ◽  
Takehiko Wada ◽  
Yuki Sarugaku ◽  
Naofumi Fujishiro ◽  
...  
Keyword(s):  
Wavelength Region ◽  
Infrared Camera ◽  
Far Infrared ◽  
Performance Estimation ◽  
Resolving Power ◽  
Wide Field ◽  
Short Wavelength Region ◽  
Mid Infrared ◽  
Pointing Error ◽  
Resolution Spectrometer

The Space Infrared Telescope for Cosmology and Astrophysics (SPICA) is an astronomical mission optimized for mid- and far-infrared astronomy, envisioned for launch in the 2020s. The Mid-infrared Camera and Spectrometer (MCS) is a model instrument that covers the 5–38[Formula: see text][Formula: see text]m wavelength range and enables imaging and spectroscopic observations via four modules named WFC-S, WFC-L, HRS, and MRS. Both of the wide field camera (WFC) modules have a 5-arcmin square field of view (FOV) but cover different wavelength ranges; WFC for the short wavelength region (WFC-S) covers 5 to 24[Formula: see text][Formula: see text]m, whereas WFC for the long wavelength region (WFC-L) covers 18 to 38[Formula: see text][Formula: see text]m. The High Resolution Spectrometer (HRS) covers the 12–18[Formula: see text][Formula: see text]m range with a resolving power of 22,000–30,000, and the Mid Resolution Spectrometer (MRS) performs integral filed units spectroscopy with a 12[Formula: see text] by 8[Formula: see text] FOV. MRS simultaneously covers the 12–38[Formula: see text][Formula: see text]m range with a moderate resolving power of 720–2000. Here, we report sensitivity estimates from a detailed modeling process involving the instrument itself, the telescope, environmental conditions, and the system error budgets. We show that the WFC-S and HRS modules require an adaptive system to correct for telescope pointing error. In particular, band pass filters (BPFs) longer than 26[Formula: see text][Formula: see text]m should be developed.

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