Weak Radio Galaxies: Narrow-Band Optical Imaging

1996 ◽  
pp. 236-237
Author(s):  
René Carrillo ◽  
Irene Cruz-González
Keyword(s):  
Optical Imaging ◽  
Narrow Band ◽  
Radio Galaxies

VIS-NIR LED Illumination in Backside Circuit Edit and Optical Probing Applications

2012 ◽  
Author(s):  
Shida Tan ◽  
Richard H. Livengood ◽  
Dane Scott ◽  
Roy Hallstein ◽  
Pat Pardy ◽  
...  
Keyword(s):  
High Resolution ◽  
Image Quality ◽  
Optical Imaging ◽  
Narrow Band ◽  
Light Emitting Diode ◽  
Air Gap ◽  
Optical Image ◽  
Proof Of Concept ◽  
Light Emitting ◽  
Optical Probing

Abstract High resolution optical imaging is critical in assisting backside circuit edit (CE) and optical probing navigation. In this paper, we demonstrated improved optical image quality using VIS-NIR narrow band light emitting diode (LED) illumination in various FIB and optical probing platforms. The proof of concept was demonstrated with both common non-contact air gap lenses and solid immersion lenses (SIL).

scholarly journals Searching for Wolf-Rayet Stars in M101

2011 ◽  
Vol 7 (S279) ◽  
pp. 118-121
Author(s):  
J. L. Bibby ◽  
P. A. Crowther ◽  
A. F. J. Moffat ◽  
M. M. Shara ◽  
D. Zurek ◽  
...  
Keyword(s):  
Optical Imaging ◽  
Strong Evidence ◽  
Narrow Band ◽  
Detection Efficiency ◽  
Narrow Band Imaging ◽  
Broad Band ◽  
Core Collapse ◽  
Central Regions

AbstractWolf-Rayet (WR) stars are the evolved descendants of massive O-type stars and are considered to be progenitor candidates for Type Ib/c core-collapse supernovae (SNe). Recent results of our HST/WFC3 survey of Wolf-Rayet stars in M101 are summarised based on the detection efficiency of narrow-band optical imaging compared to broad-band methods. We show that on average 42% of WR stars, increasing to ~85% in central regions, are only detected in the narrow-band imaging. Hence, the non-detection of a WR star at the location of ~10 Type Ib/c SNe in broad-band imaging is no longer strong evidence for a non-WR progenitor channel.

scholarly journals GTC optical imaging of extremely red 5C radio galaxies at high redshift

2015 ◽  
Vol 585 ◽  
pp. A32
Author(s):  
A. Humphrey ◽  
M. Villar-Martín ◽  
P. Lagos
Keyword(s):  
Optical Imaging ◽  
High Redshift ◽  
Radio Galaxies

scholarly journals A Deep Narrow Band Imaging Search for CIVλ1548Å and HeIIλ1640Å Emission from Lyman Alpha Blobs

2013 ◽  
Vol 9 (S304) ◽  
pp. 32-33
Author(s):  
Fabrizio Arrigoni Battaia ◽  
Y. Yang ◽  
J. F. Hennawi ◽  
Y. Matsuda ◽  
T. Yamada ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Narrow Band ◽  
Narrow Band Imaging ◽  
High Redshift ◽  
Radio Galaxies ◽  
Emission Lines ◽  
Lyman Alpha ◽  
Upper Limits ◽  
Narrowband Imaging

AbstractTo study the nature of Lyα blobs (aka LABs), we conduct a deep C IV and He II narrowband imaging survey of 13 Lyα blobs located in SSA22 proto-cluster at z ~ 3.1. We reach the unprecedented sensitivity, 5σ surface brightness limit of 2.1 − 3.4 × 10−18 erg s−1 cm−2 arcsec−2 per 1 arcsec2 aperture for two emission lines. We do not detect any extended C IV and He II emission, placing strong upper limits on the He II/Lyα and C IV/Lyα line ratios. We compare our limits with data in the literature related to the nebulae associated with high-redshift radio galaxies (HzRGs) and quasars, and we recover the data by modeling the LABs as nebulosities powered by a central QSO. For further information see Arrigoni Battaia et al. (2014).

scholarly journals Weak Radio Galaxies: Narrow-Band Optical Imaging

1996 ◽  
Vol 175 ◽  
pp. 236-237
Author(s):  
René Carrillo ◽  
Irene Cruz-González
Keyword(s):  
Emission Line ◽  
Narrow Band ◽  
Radio Galaxies ◽  
Convincing Evidence ◽  
Host Galaxy ◽  
Ultraviolet Continuum ◽  
Physical Relationship ◽  
Radio Jets ◽  
Extended Radio ◽  
Extended Emission

Previous studies show that: a) radio galaxies and radio-loud quasars have emission-line gas (ELG) which is extended on scales of tenths of kiloparsecs; b) there is convincing evidence that the kinematics and excitation of the very extended emission-line gas is governed by its interaction with the outflowing radio plasma; c) the evidence for an interaction is weaker in some radio galaxies. It is argued that the ionization of the ELG may be predominantly produced by the nuclear ultraviolet continuum and the kinematics of the gas due to the gravitational potential of the host galaxy, but it is not yet known whether there is a physical relationship between the ELG and the extended radio jets.

scholarly journals Challenges and Limitations of Narrow-Band Optical Imaging for Intra-Operative Parathyroid Identification

2016 ◽  
Vol 6 (1) ◽  
pp. 14-20
Author(s):  
Laura M. Higgins ◽  
Mark C. Pierce ◽  
Tomer Davidov
Keyword(s):  
Optical Imaging ◽  
Narrow Band

Extended optical-line-emitting gas in radio galaxies - Broad-band optical, narrow-band optical, and radio imaging of a representative sample

1988 ◽  
Vol 68 ◽  
pp. 643 ◽  
Author(s):  
Stefi Alison Baum ◽  
Timothy M. Heckman ◽  
Alan Bridle ◽  
Wil J. M. van Breugel ◽  
George K. Miley
Keyword(s):  
Representative Sample ◽  
Narrow Band ◽  
Broad Band ◽  
Radio Galaxies ◽  
Radio Imaging ◽  
Optical Line

Statistical analysis of classification

1966 ◽  
Vol 24 ◽  
pp. 188-189
Author(s):  
T. J. Deeming
Keyword(s):  
Multivariate Analysis ◽  
Statistical Analysis ◽  
Classification Scheme ◽  
Analytical Procedure ◽  
Narrow Band ◽  
Scientific Research ◽  
Maximum Amount ◽  
Amount Of Information

If we make a set of measurements, such as narrow-band or multicolour photo-electric measurements, which are designed to improve a scheme of classification, and in particular if they are designed to extend the number of dimensions of classification, i.e. the number of classification parameters, then some important problems of analytical procedure arise. First, it is important not to reproduce the errors of the classification scheme which we are trying to improve. Second, when trying to extend the number of dimensions of classification we have little or nothing with which to test the validity of the new parameters.Problems similar to these have occurred in other areas of scientific research (notably psychology and education) and the branch of Statistics called Multivariate Analysis has been developed to deal with them. The techniques of this subject are largely unknown to astronomers, but, if carefully applied, they should at the very least ensure that the astronomer gets the maximum amount of information out of his data and does not waste his time looking for information which is not there. More optimistically, these techniques are potentially capable of indicating the number of classification parameters necessary and giving specific formulas for computing them, as well as pinpointing those particular measurements which are most crucial for determining the classification parameters.

Photo-electric Hβ and uvby photometry

1966 ◽  
Vol 24 ◽  
pp. 170-180
Author(s):  
D. L. Crawford
Keyword(s):  
Narrow Band ◽  
Line Strength ◽  
Interference Filter ◽  
B Stars ◽  
Relative Line ◽  
The Mean ◽  
F Stars ◽  
Two Parameters ◽  
Filter Photometry ◽  
The Continuum

Early in the 1950's Strömgren (1, 2, 3, 4, 5) introduced medium to narrow-band interference filter photometry at the McDonald Observatory. He used six interference filters to obtain two parameters of astrophysical interest. These parameters he calledlandc, for line and continuum hydrogen absorption. The first measured empirically the absorption line strength of Hβby means of a filter of half width 35Å centered on Hβand compared to the mean of two filters situated in the continuum near Hβ. The second index measured empirically the Balmer discontinuity by means of a filter situated below the Balmer discontinuity and two above it. He showed that these two indices could accurately predict the spectral type and luminosity of both B stars and A and F stars. He later derived (6) an indexmfrom the same filters. This index was a measure of the relative line blanketing near 4100Å compared to two filters above 4500Å. These three indices confirmed earlier work by many people, including Lindblad and Becker. References to this earlier work and to the systems discussed today can be found in Strömgren's article inBasic Astronomical Data(7).

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