Monitoring the Dusty S-cluster Object (DSO/G2) on its Orbit toward the Galactic Center Black Hole

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F15%3A00441745" target="_blank" >RIV/67985815:_____/15:00441745 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/800/2/125" target="_blank" >http://dx.doi.org/10.1088/0004-637X/800/2/125</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/800/2/125" target="_blank" >10.1088/0004-637X/800/2/125</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Monitoring the Dusty S-cluster Object (DSO/G2) on its Orbit toward the Galactic Center Black Hole

Popis výsledku v původním jazyce

We analyze and report in detail new near-infrared (1.45-2.45 ?m) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with the ESO Very Large Telescope/SINFONI between2014 February and September. Before 2014 May we detect spatially compact Br? and Pa? line emission from the DSO at about 40 mas east of Sgr A*. The velocity of the source, measured from the redshifted emission, is 2700 60 km s?1. No blueshifted emissionabove the noise level is detected at the position of Sgr A* or upstream of the presumed orbit. We do not detect any significant extension of the velocity gradient across the source. We find a Br? line FWHM of 50 10 ? before and 15 10 ? after the peribothron transit, i.e., no significant line broadening with respect to last year is observed. Br? line maps show that the bulk of the line emission originates from a region of less than 20 mas diameter. This is consistent with a very compact

Název v anglickém jazyce

Monitoring the Dusty S-cluster Object (DSO/G2) on its Orbit toward the Galactic Center Black Hole

Popis výsledku anglicky

We analyze and report in detail new near-infrared (1.45-2.45 ?m) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with the ESO Very Large Telescope/SINFONI between2014 February and September. Before 2014 May we detect spatially compact Br? and Pa? line emission from the DSO at about 40 mas east of Sgr A*. The velocity of the source, measured from the redshifted emission, is 2700 60 km s?1. No blueshifted emissionabove the noise level is detected at the position of Sgr A* or upstream of the presumed orbit. We do not detect any significant extension of the velocity gradient across the source. We find a Br? line FWHM of 50 10 ? before and 15 10 ? after the peribothron transit, i.e., no significant line broadening with respect to last year is observed. Br? line maps show that the bulk of the line emission originates from a region of less than 20 mas diameter. This is consistent with a very compact

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GC13-00070J" target="_blank" >GC13-00070J: Proces akrece v silné gravitaci jádra Galaxie</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2015

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

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Svazek periodika

800

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

21

Strana od-do

"125/1"-"125/21"

Kód UT WoS článku

000349782500048

EID výsledku v databázi Scopus

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