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Publication

The infrared-radio correlation of star-forming galaxies is strongly M-star-dependent but nearly redshift-invariant since z similar to 4

Salim Bennouna, Shan Jin, Mark Thomas Sargent
2021
Journal Articles

Abstract

Over the past decade, several works have used the ratio between total (rest 8-1000 mu m) infrared and radio (rest 1.4 GHz) luminosity in star-forming galaxies (q(IR)), often referred to as the infrared-radio correlation (IRRC), to calibrate the radio emission as a star formation rate (SFR) indicator. Previous studies constrained the evolution of q(IR) with redshift, finding a mild but significant decline that is yet to be understood. Here, for the first time, we calibrate q(IR) as a function of both stellar mass (M-star) and redshift, starting from an M-star-selected sample of > 400 000 star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J) colours, at redshifts of 0.1

Official source

Salim Bennouna, Shan Jin, Mark Thomas Sargent
2021
Journal Articles

Abstract

Official source

Ontological neighbourhood

Astronomy

Astrophysics: Stellar astronomy

Related concepts (32)

Star formation

Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as "stellar nurseries" or "star-forming regions", collapse and form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy.

Star

A star is an astronomical object comprising a luminous spheroid of plasma held together by self-gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night; their immense distances from Earth make them appear as fixed points of light. The most prominent stars have been categorised into constellations and asterisms, and many of the brightest stars have proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations.

Galaxy formation and evolution

The study of galaxy formation and evolution is concerned with the processes that formed a heterogeneous universe from a homogeneous beginning, the formation of the first galaxies, the way galaxies change over time, and the processes that have generated the variety of structures observed in nearby galaxies. Galaxy formation is hypothesized to occur from structure formation theories, as a result of tiny quantum fluctuations in the aftermath of the Big Bang.

Related publications (43)

The infrared-radio correlation of star-forming galaxies is strongly M-star-dependent but nearly redshift-invariant since z similar to 4

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Evolution of the UV slope of galaxies at cosmic morning (z > 4): The properties of extremely blue galaxies

Distinct origins of environmentally quenched galaxies in the core and outer virialised regions of massive clusters at 0.8 &lt; z &lt; 1.5

BEACON: JWST NIRCam Pure-parallel Imaging Survey. I. Survey Design and Initial Results

The infrared-radio correlation of star-forming galaxies is strongly M-star-dependent but nearly redshift-invariant since z similar to 4

Evolution of the UV slope of galaxies at cosmic morning (z > 4): The properties of extremely blue galaxies

Distinct origins of environmentally quenched galaxies in the core and outer virialised regions of massive clusters at 0.8 &amp;lt; z &amp;lt; 1.5

BEACON: JWST NIRCam Pure-parallel Imaging Survey. I. Survey Design and Initial Results

Distinct origins of environmentally quenched galaxies in the core and outer virialised regions of massive clusters at 0.8 < z < 1.5