The Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII): An Experiment for High Angular Resolution in the Far-Infrared

2014 ◽  
pp. 000-000 ◽  
Author(s):  
S. A. Rinehart ◽  
M. Rizzo ◽  
D. J. Benford ◽  
D. J. Fixsen ◽  
T. J. Veach ◽  
...  
Keyword(s):  
Angular Resolution ◽  
Far Infrared ◽  
High Angular Resolution ◽  
Infrared Interferometry

High angular resolution far-infrared observations of the W3 region

1980 ◽  
Vol 242 ◽  
pp. 601 ◽  
Author(s):  
M. W. Werner ◽  
E. E. Becklin ◽  
I. Gatley ◽  
G. Neugebauer ◽  
K. Sellgren ◽  
...  
Keyword(s):  
Angular Resolution ◽  
Far Infrared ◽  
High Angular Resolution ◽  
Infrared Observations

scholarly journals The impact of clustering and angular resolution on far-infrared and millimeter continuum observations

2017 ◽  
Vol 607 ◽  
pp. A89 ◽  
Author(s):  
Matthieu Béthermin ◽  
Hao-Yi Wu ◽  
Guilaine Lagache ◽  
Iary Davidzon ◽  
Nicolas Ponthieu ◽  
...  
Keyword(s):  
Flux Density ◽  
Galaxy Evolution ◽  
Angular Resolution ◽  
Power Spectra ◽  
Far Infrared ◽  
High Angular Resolution ◽  
Strong Impact ◽  
Large Set ◽  
Number Counts ◽  
The Impact

Follow-up observations at high-angular resolution of bright submillimeter galaxies selected from deep extragalactic surveys have shown that the single-dish sources are comprised of a blend of several galaxies. Consequently, number counts derived from low- and high-angular-resolution observations are in tension. This demonstrates the importance of resolution effects at these wavelengths and the need for realistic simulations to explore them. We built a new 2 deg2 simulation of the extragalactic sky from the far-infrared to the submillimeter. It is based on an updated version of the 2SFM (two star-formation modes) galaxy evolution model. Using global galaxy properties generated by this model, we used an abundance-matching technique to populate a dark-matter lightcone and thus simulate the clustering. We produced maps from this simulation and extracted the sources, and we show that the limited angular resolution of single-dish instruments has a strong impact on (sub)millimeter continuum observations. Taking into account these resolution effects, we are reproducing a large set of observables, as number counts and their evolution with redshift and cosmic infrared background power spectra. Our simulation consistently describes the number counts from single-dish telescopes and interferometers. In particular, at 350 and 500 μm, we find that the number counts measured by Herschel between 5 and 50 mJy are biased towards high values by a factor ~2, and that the redshift distributions are biased towards low redshifts. We also show that the clustering has an important impact on the Herschel pixel histogram used to derive number counts from P(D) analysis. We find that the brightest galaxy in the beam of a 500 μm Herschel source contributes on average to only ~60% of the Herschel flux density, but that this number will rise to ~95% for future millimeter surveys on 30 m-class telescopes (e.g., NIKA2 at IRAM). Finally, we show that the large number density of red Herschel sources found in observations but not in models might be an observational artifact caused by the combination of noise, resolution effects, and the steepness of color- and flux density distributions. Our simulation, called Simulated Infrared Dusty Extragalactic Sky (SIDES), is publicly available.

High angular resolution far-infrared observations of Sagittarius B2

1992 ◽  
Vol 389 ◽  
pp. 338 ◽  
Author(s):  
Paul F. Goldsmith ◽  
Dariusz C. Lis ◽  
D. F. Lester ◽  
P. M. Harvey
Keyword(s):  
Angular Resolution ◽  
Far Infrared ◽  
High Angular Resolution ◽  
Infrared Observations

scholarly journals Star Formation at High Angular Resolution: Summary and Outlook

2004 ◽  
Vol 221 ◽  
pp. 481-485 ◽  
Author(s):  
Hans Zinnecker
Keyword(s):  
Star Formation ◽  
Numerical Simulations ◽  
Information Transfer ◽  
Information Overload ◽  
Angular Resolution ◽  
Transfer Efficiency ◽  
High Angular Resolution ◽  
Future Directions ◽  
Infrared Interferometry ◽  
Power Point

I give a personal summary of IAU-Symposium 221 “Star Formation at High Angular Resolution”, including general impressions and scientific highlights (both observations and theory). Some future directions, like infrared interferometry and advanced SPH numerical simulations, are described. In passing, I also make some critical comments about information overload and the dangers of decreasing information transfer efficiency in the age of power-point.

INTRODUCTION

2013 ◽  
Vol 02 (02) ◽  
pp. 1303001 ◽  
Author(s):  
T. TEN BRUMMELAAR ◽  
P. TUTHILL ◽  
G. VAN BELLE
Keyword(s):  
Near Infrared ◽  
Angular Resolution ◽  
The United States ◽  
High Angular Resolution ◽  
State University ◽  
Observational Astronomy ◽  
Georgia State University ◽  
Infrared Interferometry ◽  
Optical Astronomy ◽  
Modern Instrumentation

After nearly one and a half centuries of effort, one of the most pernicious problems in observational astronomy — obtaining resolved images of the stars — is finally yielding to advances in modern instrumentation. The exquisite precision delivered by today's interferometric observatories is rapidly being applied to more and more branches of optical astronomy. The most capable interferometers in the Northern Hemisphere, both located in the United States are the Navy Precision Optical Interferometer (NPOI) in Arizona and the Center for High Angular Resolution Astronomy Array (CHARA) run by Georgia State University and located in California. In early 2013 these two groups held a joint meeting hosted by the Lowell Observatory in Flagstaff. All major groups working in the field were represented at this meeting and it was suggested to us by this Journal that this was an excellent opportunity to put together a special issue on interferometry. In order to be as broad as possible, those who did not attend the CHARA/NPOI meeting were also solicited to make a contribution. The result is this collection of papers representing a snap shot of the state of the art of ground based optical and near infrared interferometry.

High angular resolution observations of AGB stars

2018 ◽  
Vol 14 (S343) ◽  
pp. 141-149
Author(s):  
Eric Lagadec
Keyword(s):  
Mass Loss ◽  
Angular Resolution ◽  
Convective Motion ◽  
High Angular Resolution ◽  
Dust Formation ◽  
Agb Stars ◽  
Chemical Enrichment ◽  
Intermediate Mass Stars ◽  
Infrared Interferometry ◽  
The Impact

AbstractMass loss of AGB stars is a key process for the late stages of evolution of low and intermediate mass stars and the chemical enrichment of galaxies. It is not fully understood yet, as it is the result of a complex combination of pulsation, convection, chemistry, shocks and dust formation.In this review I present what high angular resolution observations can teach us about this mass-loss process. Instruments such as SPHERE/VLT, Gravity and AMBER at the VLTI, and ALMA give us the possibility to map AGB stars from the optical to millimetre wavelengths with resolutions down to 1 milliarcsec. Moving from the surface of the star outwards, I present how high angular resolution observations can now produce images of the surface of the closest AGB stars and study convective motion at their surfaces, map their extended molecular atmospheres and the seeds for dust. The dust formation zone can also be mapped and its dust content characterized with mid-infrared interferometry, while ALMA can map the gas and its kinematics. I will conclude by showing how high angular resolution can help us study the impact of a companion on mass loss.

Small-Angle Electron Scattering (SAES) of Polymers

1985 ◽  
Vol 43 ◽  
pp. 78-79
Author(s):  
Ralph Oralor ◽  
Pamela Lloyd ◽  
Satish Kumar ◽  
W. W. Adams
Keyword(s):  
Electron Scattering ◽  
Small Angle ◽  
Angular Resolution ◽  
Structural Features ◽  
Objective Lens ◽  
High Angular Resolution ◽  
Push Button ◽  
First Case ◽  
Diffraction Mode ◽  
Very High

Small angle electron scattering (SAES) has been used to study structural features of up to several thousand angstroms in polymers, as well as in metals. SAES may be done either in (a) long camera mode by switching off the objective lens current or in (b) selected area diffraction mode. In the first case very high camera lengths (up to 7Ø meters on JEOL 1Ø ØCX) and high angular resolution can be obtained, while in the second case smaller camera lengths (approximately up to 3.6 meters on JEOL 1Ø ØCX) and lower angular resolution is obtainable. We conducted our SAES studies on JEOL 1ØØCX which can be switched to either mode with a push button as a standard feature.

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