scholarly journals Does the fir-radio correlation evolve with redshift in irregular and disk galaxies?

2021 ◽  
pp. 15-27
Author(s):  
M.S. Pavlovic
Keyword(s):  
Fundamental Problem ◽  
Far Infrared ◽  
Morphological Type ◽  
Disk Galaxies ◽  
Massive Galaxies ◽  
Star Forming ◽  
Optical Images ◽  
Thermal Radio Emission ◽  
Irregular Galaxies ◽  
Strong Linear Correlation

It was confirmed that there is a strong linear correlation between the thermal far-infrared (FIR) and non-thermal radio emission of the star-forming galaxies. Recent works based on this correlation over large redshifts have shown that the correlation is evolving towards higher redshifts. In this paper, possible physical causes that lead to the evolution of this correlation are explored. One possible cause is that the interaction between galaxies is responsible for this behavior. We used the morphology of galaxies, as an indicator of past or present interactions, because it is generally known that the irregular morphology of galaxies is a consequence of collisions or close approaches. To test this hypothesis, a sample of dusty star-forming galaxies up to a redshift z = 3:5 from the COSMOS field has been selected. The sample has been divided, according to the morphological type, into two subsamples (disk and irregular galaxies), and the evolution of the correlation with redshift has been analyzed separately for both of them. It was found that in both subsamples there is no indication for the redshift evolution of the FIR-radio correlation. However, it was also found that the mean correlation parameter, qFIR, is lower in irregular galaxies, which may indicate that they can still affect the evolution of the correlation if their abundance in the sample increases towards higher redshifts. Disk galaxies, which statistically dominate the sample, may be responsible for the lack of this evolution. On the other hand, a fundamental problem with optically determined morphology is the dust obscuration in massive galaxies at z > 2. To test the idea that interacting galaxies are responsible for redshift evolution of the FIR-radio correlation, it is, necessary to analyze a much larger sample for which the morphology has been determined, taking into account the VLA and ALMA imaging in addition to optical images, and which contains a higher fraction of irregular galaxies. Finally, it was also found that the qFIR parameter and its evolution are very sensitive to the radio spectral index above z > 1 and that its misinterpretation and taking a constant value of ? = 0:7 may be responsible for the observed evolution of the correlation.

scholarly journals What is driving the evolution of the far-infrared radio correlation?

2019 ◽  
pp. 9-16
Author(s):  
Marina Pavlovic ◽  
Tijana Prodanovic
Keyword(s):  
Radio Emission ◽  
Large Range ◽  
High Redshift ◽  
Far Infrared ◽  
Morphological Type ◽  
Interacting Galaxies ◽  
Disk Galaxies ◽  
Star Forming ◽  
Submillimeter Galaxies ◽  
Small Dispersion

Far infrared-radio correlation represents a linear relationship between far-infrared (FIR) and radio emission in star-forming galaxies. Previous observations have confirmed that this correlation is maintained over a large range of redshift and does not evolve, although a small dispersion is present. However, some of more recent observations at high redshift have shown the opposite. The question that arises is - what is driving this evolution? In this paper we investigate the possibility that galaxy morphology is the answer to this question. A sample of 37 submillimeter galaxies (SMGs) is analyzed. The observation and morphological class of these galaxies has previously been published. We examined FIR-radio correlation in galaxies of different morphological type in this sample and found that for star-forming disk galaxies correlation is stable and does not evolve and for irregular and interacting galaxies we find some hints of evolution.

scholarly journals Far-Infrared Emission from Clumpy Irregular Galaxies

1987 ◽  
Vol 115 ◽  
pp. 647-647
Author(s):  
U. Klein ◽  
J. Heidmann ◽  
R. Wielebinski ◽  
E. Wunderlich
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Hubble Constant ◽  
Far Infrared ◽  
Hii Regions ◽  
Infrared Emission ◽  
Star Forming ◽  
Irregular Galaxies

The four clumpy irregular galaxies Mkr 8, 296,297 and 325 have been observed by IRAS. All galaxies have been detected in at least two of the four detector bands. The ratios of the 100 to 60-m flux densities are comparable to those of HII regions or violently star forming galaxies. The average star formation rate in clumpy irregular galaxies is of the order of a few solar masses per year (based on their average far-infrared luminosity and a Hubble constant of 75 km s−1 Mpc−1.

scholarly journals Galaxies hosting an active galactic nucleus: a view from the CALIFA survey

2020 ◽  
Vol 492 (3) ◽  
pp. 3073-3090 ◽  
Author(s):  
Eduardo A D Lacerda ◽  
Sebastián F Sánchez ◽  
R Cid Fernandes ◽  
Carlos López-Cobá ◽  
Carlos Espinosa-Ponce ◽  
...  
Keyword(s):  
Star Formation ◽  
Morphological Type ◽  
Molecular Gas ◽  
Main Role ◽  
Type I ◽  
Massive Galaxies ◽  
Star Forming ◽  
Integral Field Spectroscopy ◽  
Almost All ◽  
Formation Efficiency

ABSTRACT We study the presence of optically-selected active galactic nuclei (AGNs) within a sample of 867 galaxies extracted from the extended Calar-Alto Legacy Integral Field spectroscopy Area (eCALIFA) spanning all morphological classes. We identify 10 Type-I and 24 Type-II AGNs, amounting to ∼4 per cent of our sample, similar to the fraction reported by previous explorations in the same redshift range. We compare the integrated properties of the ionized and molecular gas, and stellar population of AGN hosts and their non-active counterparts, combining them with morphological information. The AGN hosts are found in transitory parts (i.e. green-valley) in almost all analysed properties which present bimodal distributions (i.e. a region where reside star-forming galaxies and another with quiescent/retired ones). Regarding morphology, we find AGN hosts among the most massive galaxies, with enhanced central stellar-mass surface density in comparison to the average population at each morphological type. Moreover, their distribution peaks at the Sab-Sb classes and none are found among very late-type galaxies (>Scd). Finally, we inspect how the AGN could act in their hosts regarding the quenching of star-formation. The main role of the AGN in the quenching process appears to be the removal (or heating) of molecular gas, rather than an additional suppression of the already observed decrease of the star-formation efficiency from late-to-early type galaxies.

scholarly journals A correlation between star formation rate and average black hole accretion rate in star forming galaxies

2013 ◽  
Vol 9 (S304) ◽  
pp. 302-306
Author(s):  
Chien-Ting J. Chen ◽  
Ryan C. Hickox
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Star Formation Rate ◽  
Accretion Rate ◽  
Formation Rate ◽  
Far Infrared ◽  
Host Galaxies ◽  
Star Forming ◽  
Black Hole Accretion ◽  
Strong Linear Correlation

AbstractWe present the results of recent studies on the co-evolution of galaxies and the supermassive black holes (SMBHs) using Herschel far-infrared and Chandra X-ray observations in the Boötes survey region. For a sample of star-forming (SF) galaxies, we find a strong correlation between galactic star formation rate and the average SMBH accretion rate in SF galaxies. Recent studies have shown that star formation and AGN accretion are only weakly correlated for individual AGN, but this may be due to the short variability timescale of AGN relative to star formation. Averaging over the full AGN population yields a strong linear correlation between accretion and star formation, consistent with a simple picture in which the growth of SMBHs and their host galaxies are closely linked over galaxy evolution time scales.

scholarly journals Far-infrared and sub-millimeter properties of SDSS galaxies in the Herschel ATLAS SDP Field

2011 ◽  
Vol 7 (S284) ◽  
pp. 286-288
Author(s):  
Man I. Lam ◽  
Hong Wu ◽  
Yi-Nan Zhu
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Stellar Population ◽  
Far Infrared ◽  
Morphological Type ◽  
Dust Grains ◽  
Space Observatory ◽  
Star Forming ◽  
Using Data ◽  
Cold Dust

AbstractUsing data from the new infrared facility the Herschel Space Observatory, we have analyzed correlations between morphological type, far-infrared (FIR) luminosity, and Hα luminosity for star-forming galaxies, composite galaxies, and AGNs. We found a trend in scatter from 100μm to 500μm, which indicates that the submillimeter bands are not a good star formation tracer in these galaxies, being contaminated either by the old stellar population or by the interstellar medium (ISM). AGNs have no significant effect on our fitting results since the far-infrared to submillimeter emission is from cold dust/large dust grains.

scholarly journals Spatially resolved dynamics of high-z star forming galaxies

2008 ◽  
Vol 4 (S254) ◽  
pp. 33-34
Author(s):  
Reinhard Genzel
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Adaptive Optics ◽  
Disk Galaxies ◽  
Massive Galaxies ◽  
Star Forming ◽  
Secular Evolution ◽  
Spatially Resolved ◽  
The Impact ◽  
Integral Field

AbstractI report on two major programs to study the kinematic properties of galaxies at z ~ 1.5 − 3 with spatially resolved spectroscopy for the first time. Using the adaptive optics assisted, integral field spectrometer SINFONI on the ESO VLT, we have observed more than 70 galaxies and find compelling evidence for large, geometrically thick (turbulent), rotating disk galaxies in a majority of the objects that we can spatially resolve. It appears that these star forming disks are driven by continuous, rapid accretion of gas from their dark matter halos, and that their evolution is strongly influenced by internal, secular evolution. In contrast to the 20 submillimeter galaxies that we have investigated with the IRAM Plateau de Bure millimetre interferometer we find strong evidence for compact, major mergers. I discuss the impact of these new observations on our understanding of galaxy evolution in the early Universe.For the SINS survey we have carried out Hα integral field spectroscopy of well-resolved, UV/optically selected star-forming galaxies at z ~ 2 with SINFONI on the ESO VLT. The SINS sample is representative of the majority of massive (M* > a few 1010M⊙) star-forming galaxies at that redshift. Our data obtained with laser guide star assisted adaptive optics in good seeing show the presence of turbulent, rotating star-forming rings/disks in at least a third of the sample, plus central bulge/inner disk components in some of the best cases, whose mass fractions relative to total dynamical mass appears to scale with [NII]/Hα flux ratio and ‘star formation’ age. Another third of the SINS galaxies show clear signs of kinematic perturbations by a merger, while the last third appear to be compact, ‘dispersion’ limited systems.Our interpretation of these data is that the buildup of the central disks and bulges of massive galaxies at z ~ 2 can be driven by the early secular evolution of gas-rich ‘proto’-disks. High-redshift disks exhibit large random motions. This turbulence may in part be stirred up by the release of gravitational energy in the rapid ‘cold’ accretion flows along the filaments of the cosmic web. As a result, dynamical friction and viscous processes proceed on a time scale of < 1 Gyr, at least an order of magnitude faster than in disk galaxies at z ~ 0. Early secular evolution thus drives gas and stars into the central regions and can build up exponential disks and massive bulges, even without major mergers. Secular evolution along with increased efficiency of star formation at high surface densities may also help to account for the short time scales of the stellar buildup observed in massive galaxies at z ~ 2.

scholarly journals The ALPINE-ALMA [CII] survey

2020 ◽  
Vol 643 ◽  
pp. A4 ◽  
Author(s):  
Y. Fudamoto ◽  
P. A. Oesch ◽  
A. Faisst ◽  
M. Béthermin ◽  
M. Ginolfi ◽  
...  
Keyword(s):  
Star Formation ◽  
Far Infrared ◽  
Systematic Change ◽  
Attenuation Curve ◽  
Infrared Excess ◽  
Massive Galaxies ◽  
Star Forming ◽  
Large Program ◽  
The Individual ◽  
Dust Attenuation

We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 − 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M⋆), and infrared excess (IRX = LIR/LUV). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 − 5.8. The individual detections and stacks show that the IRX–β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z <  4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX–β relation as a function of redshift suggests an evolution of dust attenuation properties at z >  4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX–M⋆ relations at z ≲ 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z ≳ 4 are characterised by (i) a steeper attenuation curve than at z ≲ 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M⋆/M⊙ >  10) at z ∼ 5 − 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.

scholarly journals Impact of galactic interactions on the evolution of the far-infrared–radio correlation

2019 ◽  
Vol 489 (4) ◽  
pp. 4557-4564
Author(s):  
M Pavlović ◽  
T Prodanović
Keyword(s):  
Radio Emission ◽  
Strong Correlation ◽  
Far Infrared ◽  
Small Sample ◽  
Star Forming ◽  
Redshift Surveys ◽  
Irregular Galaxies

ABSTRACT A strong correlation has been known to exist between the far-infrared (FIR) and radio emission of star-forming galaxies. Observations have shown that, although scatter is present, this correlation holds over a range of redshifts and does not evolve. However, there have been a number of more recent observations, especially in higher redshift surveys, indicating the opposite. The question that then presents itself is: what is driving this evolution? In this work, we explore the possibility that the answer might be hiding in galactic interactions and revealed by morphology. We present a number of models based on the evolving number of galaxies of different morphological types, some of which could potentially explain the observed trends and scatter in general. Furthermore, we analyse a small sample of 34 submillimetre galaxies for which observations have been published and morphology classified. In this sample, we look at the FIR–radio correlation separately in galaxies of different morphological types. We find that, while for both disc and irregular star-forming galaxies there are hints of evolution of this correlation with redshift, where this evolution appears to be stronger in irregular galaxies, due to low number statistics, both samples are also consistent with no evolution, making it difficult at this point to discriminate between models. However, when analysis was performed on the combined sample, an evolving and decreasing trend was indeed found, indicating that evolution should be expected in at least one of the morphological types.

scholarly journals Oxygen yields as a constraint on feedback processes in galaxies

2019 ◽  
Vol 490 (1) ◽  
pp. 868-888 ◽  
Author(s):  
Maritza A Lara-López ◽  
Maria Emilia De Rossi ◽  
Leonid S Pilyugin ◽  
Anna Gallazzi ◽  
Thomas M Hughes ◽  
...  
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Virgo Cluster ◽  
Massive Galaxies ◽  
Star Forming ◽  
Irregular Galaxies ◽  
Low Mass ◽  
Radio Measurements ◽  
Oxygen Yield ◽  
Baryonic Mass

ABSTRACT We study the interplay between several properties determined from optical and a combination of optical/radio measurements, such as the effective oxygen yield (yeff), the star formation efficiency, gas metallicity, depletion time, gas fraction, and baryonic mass (Mbar), among others. We use spectroscopic data from the SDSS survey, and H i information from the ALFALFA survey to build a statistically significant sample of more than 5000 galaxies. Furthermore, we complement our analysis with data from the GASS and COLD GASS surveys, and with a sample of star-forming galaxies from the Virgo cluster. Additionally, we have compared our results with predictions from the EAGLE simulations, finding a very good agreement when using the high-resolution run. We explore in detail the Mbar–yeff relation, finding a bimodal trend that can be separated when the stellar age of galaxies is considered. On one hand, yeff increases with Mbar for young galaxies [log(tr) < 9.2 yr], while yeff shows an anticorrelation with Mbar for older galaxies [log(tr) > 9.4 yr]. While a correlation between Mbar and yeff has been observed and studied before, mainly for samples of dwarfs and irregular galaxies, their anticorrelated counterpart for massive galaxies has not been previously reported. The EAGLE simulations indicate that AGN feedback must have played an important role in their history by quenching their star formation rate, whereas low-mass galaxies would have been affected by a combination of outflows and infall of gas.

Far infrared study of the giant star forming complex W 51

2002 ◽  
Vol 4 ◽  
pp. 333-333
Author(s):  
S. K. Ghosh ◽  
D. K. Ojha ◽  
R. P. Verma
Keyword(s):  
Far Infrared ◽  
Infrared Study ◽  
Giant Star ◽  
Star Forming
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