A3B5 photodiode sensors for low-temperature pyrometry

Sotnikova, G. Yu.; Александров, С. Е.; Гаврилов, Г. А.

doi:10.1117/12.886309

Cited by 25 publications

(23 citation statements)

References 1 publication

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“…In such encounters the total amount of gas transferred to the early-type object is roughly 10 per cent of the gas in the accreted spiral, i.e. up to 10 9 M (Reshetnikov & Sotnikova 1997). However, the high H I content (∼10 10 M ) detected in UGC 4599 is comparable with the entire gas content of a large spiral galaxy, and is one order of magnitude larger than the typical H I content of dwarf irregular galaxies (Matthews, Galagher & Littleton 1993;Matthews & Gallagher 1996).…”

Section: Major Accretion Eventmentioning

confidence: 99%

“…However, the central spheroid and the ring of Hoag's Object are at rest relative to each other and seem to form one single object (Schweizer et al 1987). A small fraction of ring galaxies are believed to be formed by more gentle interactions such as matter accretion from a gas-rich companion or minor mergers (Buta & Combes 1996;Reshetnikov & Sotnikova 1997). In such a scenario a polar ring galaxy (PRG) might be formed if the host galaxy, typically an S0, exhibits an outer ring of stars and interstellar matter that rotates in a plane highly inclined to the central stellar body (Whitmore et al 1990).…”

Section: Introductionmentioning

confidence: 99%

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UGC 4599: a photometric study of the nearest Hoag-type ring galaxy

Finkelman

Brosch

2011

Monthly Notices of the Royal Astronomical Society

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We present a photometric study of UGC 4599, a low‐luminosity galaxy superficially resembling Hoag's Object in that on sky survey images it appears to be a complete ring surrounding a roundish core. The nature of the outer ring of Hoag‐type galaxies is still debated and may be related either to slow secular evolution or to environmental processes, such as galaxy–galaxy interactions. As the nearest of its kind, UGC 4599 is a perfect target for a detailed study of the peculiar structure of this type of objects. Surface photometry of the central body of the ring and the ring itself was performed using GALEX, Sloan Digital Sky Survey (SDSS) and Two Micron All Sky Survey (2MASS) photometric data available online. To identify bright clumps across the ring that could be H ii regions associated with the ring we obtained images of UGC 4599 at the Wise Observatory through U‐, B‐ and R‐band and narrow‐band rest‐frame Hα filters. Although classified in HyperLEDA as S0 with an external ring, we show that in UGC 4599 (a) the nearly round central body follows well an light profile almost all the way to the centre, (b) the isophotes are strongly twisted with a sharp 45° transition at a radius of r≃ 6 arcsec, (c) the blue ring seems to have reached near‐equilibrium configuration with the central body, (d) the ring is actually composed of a one‐and‐a‐half turn spiral feature and (e) one side of the spiral shows conspicuous star formation in the form of at least nine H ii regions, revealed by their Hα emission. Based on the photometric data, together with H i information from the literature, we characterize UGC 4599 as an elliptical‐like object surrounded by a luminous ring and a massive, extremely extended H i disc. Given its observed properties, we rule out UGC 4599 as representing a late phase in barred early‐type galaxies evolution. We discuss the origin of UGC 4599 and conclude that this galaxy could be the result of a major interaction between two gas‐rich spiral galaxies that took place at least 5 Gyr ago. However, deep optical imaging and a detailed stellar population analysis are required to determine whether the large gas reservoir could have been accreted directly from the intergalactic medium on to a pre‐existing elliptical galaxy in the early Universe. A detailed kinematical study will shed light on the exact nature of the central body and the ring of UGC 4599.

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Section: Major Accretion Eventmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

UGC 4599: a photometric study of the nearest Hoag-type ring galaxy

Finkelman

Brosch

2011

Monthly Notices of the Royal Astronomical Society

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“…There is growing interest to photodiodes (PDs) with peak sensitivity around k = 3-4 lm for use in thermal imaging [1], low temperature pyrometry [2,3] and in nondispersive infrared (NDIR) analysis of hydrocarbon gases that have fundamental absorption band near the 3.4 lm wavelength. In combination with light emitting diodes (LEDs) with peak emission at 3.4 lm the above large area PDs can be used for low power consumption gas sensors and portable gas analyzers [4] while small (element) area/capacitance PDs are important for recording of fast thermal processes.…”

Section: Introductionmentioning

confidence: 99%

Low dark current P- InAsSbP /n- InAs/N-InAsSbP/n + - InAs double heterostructure back-side illuminated photodiodes

Brunkov

Il’inskaya

Karandashev

et al. 2016

Infrared Physics & Technology

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“…In the merging scenario, the PRG results from a 'polar' merger of two disc galaxies with unequal mass: the morphology and kinematics of the merger remnants depend on the merging initial orbital parameters and the initial mass ratio of the two galaxies (Bekki 1998a,b;Bournaud, Jog & Combes 2005). In the accretion scenario, the polar ring/disc may form by (i) the disruption of a dwarf companion galaxy orbiting around an early-type system or (ii) the tidal accretion of gas stripped from disc galaxy outskirts, captured by an early-type galaxy on a parabolic encounter (Reshetnikov & Sotnikova 1997;Bournaud & Combes 2003;Hancock et al 2009). The cold accretion scenario has been proposed very recently for the formation of wide disc-like polar rings: a long-lived polar structure may form through cold gas accretion along a filament, extended for ∼1 Mpc, into the virialized dark matter halo (Macciò, Moore & Stadel 2006;Brook et al 2008).…”

Section: Introductionmentioning

confidence: 99%

A new photometric investigation of the double-ringed galaxy ESO 474−G26: unveiling the formation scenario

Spavone¹,

Iodice

Bettoni

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present a detailed photometric study of the peculiar double-ringed galaxy ESO 474-G26. Near-infrared (NIR) and optical data have been used, with the main goal of constraining the formation history of ESO 474-G26. NIR photometry is fundamental in this kind of study, because it gives better constraints on the spectral energy distribution (SED) and traces the older stellar population of the galaxy well. This galaxy presents a very complex structure with two almost orthogonal rings, one in the equatorial and another in the polar plane, around an elliptical-like object. Due to the peculiar morphology of ESO 474-G26, we used both NIR images (J and K bands) to derive accurate analysis of the stellar light distribution and optical images (in the B, V and R bands) to derive colour profiles and colour maps to study the structure of the rings. The observational characteristics of ESO 474-G26 are typical of galaxies that have experienced some kind of interaction during their evolution. We investigated two alternatives: a merging process and an accretion event

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A3B5 photodiode sensors for low-temperature pyrometry

Cited by 25 publications

References 1 publication

UGC 4599: a photometric study of the nearest Hoag-type ring galaxy

UGC 4599: a photometric study of the nearest Hoag-type ring galaxy

Low dark current P- InAsSbP /n- InAs/N-InAsSbP/n + - InAs double heterostructure back-side illuminated photodiodes

A new photometric investigation of the double-ringed galaxy ESO 474−G26: unveiling the formation scenario

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