scholarly journals Compact star-forming galaxies preferentially quenched to become PSBs inz< 1 clusters

2018 ◽  
Vol 482 (2) ◽  
pp. 1640-1650 ◽  
Author(s):  
Miguel Socolovsky ◽  
David T Maltby ◽  
Nina A Hatch ◽  
Omar Almaini ◽  
Vivienne Wild ◽  
...  
Keyword(s):  
Compact Star ◽  
Star Forming

scholarly journals A pair of UV nuclei or a compact star-forming region near the active nucleus in Mrk 766?

2021 ◽  
Vol 42 (2) ◽  
Author(s):  
P. P. Deka ◽  
G. C. Dewangan ◽  
K. P. Singh ◽  
J. Postma
Keyword(s):  
Compact Star ◽  
Active Nucleus ◽  
Star Forming

scholarly journals SUB-KILOPARSEC ALMA IMAGING OF COMPACT STAR-FORMING GALAXIES AT z ∼ 2.5: REVEALING THE FORMATION OF DENSE GALACTIC CORES IN THE PROGENITORS OF COMPACT QUIESCENT GALAXIES

2016 ◽  
Vol 827 (2) ◽  
pp. L32 ◽  
Author(s):  
G. Barro ◽  
M. Kriek ◽  
P. G. Pérez-González ◽  
J. R. Trump ◽  
D. C. Koo ◽  
...  
Keyword(s):  
Compact Star ◽  
Star Forming

scholarly journals An uncertainty principle for star formation – IV. On the nature and filtering of diffuse emission

2019 ◽  
Vol 488 (2) ◽  
pp. 2800-2824 ◽  
Author(s):  
Alexander P S Hygate ◽  
J M Diederik Kruijssen ◽  
Mélanie Chevance ◽  
Andreas Schruba ◽  
Daniel T Haydon ◽  
...  
Keyword(s):  
Star Formation ◽  
Compact Star ◽  
Critical Length ◽  
Electromagnetic Spectrum ◽  
H Ii Regions ◽  
Diffuse Emission ◽  
Star Forming ◽  
Star Forming Regions ◽  
Compact Component ◽  
Astronomical Images

Abstract Diffuse emission is observed in galaxies in many tracers across the electromagnetic spectrum, including tracers of star formation, such as H α and ultraviolet (UV), and tracers of gas mass, such as carbon monoxide (CO) transition lines and the 21-cm line of atomic hydrogen (H i). Its treatment is key to extracting meaningful information from observations such as cloud-scale star formation rates. Finally, studying diffuse emission can reveal information about the physical processes taking place in the interstellar medium, such as chemical transitions and the nature of stellar feedback (through the photon escape fraction). We present a physically motivated method for decomposing astronomical images containing both diffuse emission and compact regions of interest, such as H ii regions or molecular clouds, into diffuse and compact component images through filtering in Fourier space. We have previously presented a statistical method for constraining the evolutionary timeline of star formation and mean separation length between compact star-forming regions with galaxy-scale observations. We demonstrate how these measurements are biased by the presence of diffuse emission in tracer maps and that by using the mean separation length as a critical length-scale to separate diffuse emission from compact emission, we are able to remove its biasing effect. Furthermore, this method provides, without the need for interferometry or ancillary spectral data, a measurement of the diffuse emission fraction in input tracer maps and decomposed diffuse and compact emission maps for further analysis.

scholarly journals Obscured active galactic nuclei triggered in compact star-forming galaxies

2016 ◽  
Vol 466 (1) ◽  
pp. L103-L107 ◽  
Author(s):  
Yu-Yen Chang ◽  
Emeric Le Floc'h ◽  
Stéphanie Juneau ◽  
Elisabete da Cunha ◽  
Mara Salvato ◽  
...  
Keyword(s):  
Active Galactic Nuclei ◽  
Compact Star ◽  
Galactic Nuclei ◽  
Star Forming

scholarly journals Compact star forming galaxies as the progenitors of compact quiescent galaxies: Clustering result

New Astronomy ◽  
2017 ◽  
Vol 51 ◽  
pp. 99-104
Author(s):  
Xiaozhi Lin ◽  
Lulu Fan ◽  
Xu Kong ◽  
Guanwen Fang
Keyword(s):  
Compact Star ◽  
Star Forming

scholarly journals No supernovae detected in two long-duration gamma-ray bursts

2007 ◽  
Vol 365 (1854) ◽  
pp. 1269-1275 ◽  
Author(s):  
D Watson ◽  
J.P.U Fynbo ◽  
C.C Thöne ◽  
J Sollerman
Keyword(s):  
Massive Star ◽  
Gamma Ray ◽  
Compact Star ◽  
Gamma Ray Bursts ◽  
Host Galaxy ◽  
Core Collapse ◽  
Host Galaxies ◽  
Star Forming ◽  
Long Duration ◽  
Spiral Arm

There is strong evidence that long-duration gamma-ray bursts (GRBs) are produced during the collapse of a massive star. In the standard version of the collapsar model, a broad-lined and luminous Type Ic core-collapse supernova (SN) accompanies the GRB. This association has been confirmed in observations of several nearby GRBs. Recent observations show that some long-duration GRBs are different. No SN emission accompanied the long-duration GRBs 060505 and 060614 down to limits fainter than any known Type Ic SN and hundreds of times fainter than the archetypal SN 1998bw that accompanied GRB 980425. Multi-band observations of the early afterglows, as well as spectroscopy of the host galaxies, exclude the possibility of significant dust obscuration. Furthermore, the bursts originated in star-forming galaxies, and in the case of GRB 060505, the burst was localized to a compact star-forming knot in a spiral arm of its host galaxy. We find that the properties of the host galaxies, the long duration of the bursts and, in the case of GRB 060505, the location of the burst within its host, all imply a massive stellar origin. The absence of an SN to such deep limits therefore suggests a new phenomenological type of massive stellar death.

scholarly journals Wind of a young massive star colliding with a supernova remnant shell

2021 ◽  
Vol 2103 (1) ◽  
pp. 012013
Author(s):  
D V Badmaev ◽  
A M Bykov
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Massive Star ◽  
Compact Star ◽  
Complex Structure ◽  
Stellar Winds ◽  
Star Forming ◽  
Star Forming Regions ◽  
Supernova Shell ◽  
Favorable Conditions

Abstract The fast stellar winds of massive stars, along with supernovae, determine the dynamics within the star-forming regions. Within a compact star cluster, counterpropagating supersonic MHD shock flows associated with winds and supernova remnants can provide favorable conditions for efficient Fermi I particle acceleration up to energies > 10 PeV over a short timescale of several hundred years. To model the nonthermal spectra of such systems it is necessary to know the complex structure of colliding supersonic flows. In this paper using the PLUTO code we study on a subparsec scale a 2D MHD model of the collision of a core-collapse supernova remnant with a magnetized wind of a hot rotating O-star. As a result the detailed high resolution (~ 10−4 pc) maps of density, magnetic field, and temperature during the the wind - supernova shell interaction are presented.

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