The bivariate<i>K</i>-band-submillimetre luminosity functions of the local HRS galaxy sample

Andreani, P.; Spinoglio, L.; Boselli, A.; Ciesla, L.; Cortese, Luca; Vio, R.; Baes, M.; Bendo, G. J.

doi:10.1051/0004-6361/201322747

Cited by 11 publications

(25 citation statements)

References 51 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…At first sight, this systematic difference is somewhat unexpected, as our EAGLE-SKIRT post-processing recipe is primarily calibrated based on SPIRE data (Camps et al 2016). However, the HRS galaxies used in the calibration process are all normal latetype star-forming galaxies, which populate the low-luminosity side of the luminosity function (Andreani et al 2014). This explains the excellent agreement between EAGLE-SKIRT and HerMES in his regime, but also leaves the high-luminosity tail unconstrained.…”

Section: Submm Luminosity Functionsmentioning

confidence: 99%

Infrared luminosity functions and dust mass functions in the EAGLE simulation

Baes

Trčka

Camps

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present infrared luminosity functions and dust mass functions for the EAGLE cosmological simulation, based on synthetic multi-wavelength observations generated with the SKIRT radiative transfer code. In the local Universe, we reproduce the observed infrared luminosity and dust mass functions very well. Some minor discrepancies are encountered, mainly in the high luminosity regime, where the EAGLE-SKIRT luminosity functions mildly but systematically underestimate the observed ones. The agreement between the EAGLE-SKIRT infrared luminosity functions and the observed ones gradually worsens with increasing lookback time. Fitting modified Schechter functions to the EAGLE-SKIRT luminosity and dust mass functions at different redshifts up to z = 1, we find that the evolution is compatible with pure luminosity/mass evolution. The evolution is relatively mild: within this redshift range, we find an evolution of L ,250 ∝ (1 + z) 1.68 , L ,TIR ∝ (1 + z) 2.51 and M ,dust ∝ (1 + z) 0.83 for the characteristic luminosity/mass. For the luminosity/mass density we find ε 250 ∝ (1 + z) 1.62 , ε TIR ∝ (1 + z) 2.35 and ρ dust ∝ (1 + z) 0.80 , respectively. The mild evolution of the dust mass density is in relatively good agreement with observations, but the slow evolution of the infrared luminosity underestimates the observed luminosity evolution significantly. We argue that these differences can be attributed to increasing limitations in the radiative transfer treatment due to increasingly poorer resolution, combined with a slower than observed evolution of the SFR density in the EAGLE simulation and the lack of AGN emission in our EAGLE-SKIRT post-processing recipe.

show abstract

Section: Submm Luminosity Functionsmentioning

confidence: 99%

Infrared luminosity functions and dust mass functions in the EAGLE simulation

Baes

Trčka

Camps

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This data set has been extensively used to investigate many aspects of the physics of the interstellar medium, among others the stellar, dust, gas mass functions, infrared luminosity function, and the star formation function (Cortese et al 2012;Boselli et al 2010Boselli et al , 2014aBoselli et al ,b, 2015Ciesla et al 2014;Andreani et al 2014Andreani et al , 2018.…”

Section: The Datamentioning

confidence: 99%

“…We have recently investigated the HRS LFs and MFs using the bivariate functions with respect to the K-band luminosity, which is the band at which the sample is complete (Andreani et al 2014(Andreani et al , 2018. We have employed an accurate statistical method which makes use of the entire data sets including the upper limits.…”

Section: The Datamentioning

confidence: 99%

“…The survey selection criteria (magnitude-and volumelimited, see Sect. 2), size and multiwavelength coverage (from UV to radio wavelengths both in spectroscopy and photometry), together with the Herschel results in the FIR, which are sensitive to dust mass down to 10 4 M , have shown that the HRS can be considered as a 'reference' sample to carry out a statistical analysis in the local Universe (Boselli et al 2010;Andreani et al 2014Andreani et al , 2018.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The molecular mass function of the local Universe

Andreani

Miyamoto

Kaneko

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We construct the molecular mass function using the bivariate K-band-mass function (BMF) of the Herschel Reference Survey (HRS), which is a volume-limited sample that has already been widely studied at the entire electromagnetic spectrum. Methods. The molecular mass function was derived from the K-band and the gas mass cumulative distribution using a copula method, which is described in detail in our previous papers. Results. The H2 mass is relatively strongly correlated with the K-band luminosity because of the tight relation between the stellar mass and the molecular gas mass within the sample with a scatter, which is likely due to those galaxies which have lost their molecular content because of environmental effects or because of a larger gas consumption due to past star formation processes. The derived H2 MF samples the molecular mass range from ∼4 × 106 M⊙ to ∼1010 M⊙, and when compared with theoretical models, it agrees well with the theoretical predictions at the lower end of the mass values; whereas at masses larger than 1010 M⊙, the HRS sample may miss galaxies with a large content of molecular hydrogen and the outcomes are not conclusive. The value of the local density of the molecular gas mass inferred from our analysis is ∼1.5 × 107 M⊙ Mpc−3, and it is compared with the results at larger redshifts, confirming the lack of strong evolution for the molecular mass density between z = 0 and z = 4. Conclusions. This is the first molecular mass function that has been derived on a complete sample in the local Universe, which can be used as a reliable calibration at redshift z = 0 for models aiming to predict the evolution of the molecular mass density.

show abstract

“…In cosmology, 2D copulas have been used by Scherrer et al (2010) for the determination of the PDF of the density field of the large-scale structure of the Universe, by Lin & Kilbinger (2015) and Lin et al (2016) to predict weak-lensing peak counts, and by Sato et al (2010Sato et al ( , 2011 for the precise estimation of cosmological parameters. Other astronomical applications include the determination of the far-UV (FUV) and far-IR bivariate luminosity function of galaxies (Takeuchi 2010;Takeuchi et al 2011), the determination of the K-band and the submillimeter luminosity function (Andreani et al 2014), and the bivariate luminosity versus the mass functions of the of the local HRS galaxy sample (Andreani et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Modeling high-dimensional dependence in astronomical data

Vio¹,

Nagler

Andreani³

2020

A&A

Self Cite

View full text Add to dashboard Cite

Fixing the relationship of a set of experimental quantities is a fundamental issue in many scientific disciplines. In the 2D case, the classical approach is to compute the linear correlation coefficient ρ from a scatterplot. This method, however, implicitly assumes a linear relationship between the variables. Such an assumption is not always correct. With the use of the partial correlation coefficients, an extension to the multidimensional case is possible. However, the problem of the assumed mutual linear relationship of the variables remains. A relatively recent approach that makes it possible to avoid this problem is the modeling of the joint probability density function of the data with copulas. These are functions that contain all the information on the relationship between two random variables. Although in principle this approach also can work with multidimensional data, theoretical as well computational difficulties often limit its use to the 2D case. In this paper, we consider an approach based on so-called vine copulas, which overcomes this limitation and at the same time is amenable to a theoretical treatment and feasible from the computational point of view. We applied this method to published data on the near-IR and far-IR luminosities and atomic and molecular masses of the Herschel reference sample, a volume-limited sample in the nearby Universe. We determined the relationship of the luminosities and gas masses and show that the far-IR luminosity can be considered as the key parameter relating the other three quantities. Once removed from the 4D relation, the residual relation among the latter is negligible. This may be interpreted as the correlation between the gas masses and near-IR luminosity being driven by the far-IR luminosity, likely by the star formation activity of the galaxy.

show abstract

The bivariateK-band-submillimetre luminosity functions of the local HRS galaxy sample

Cited by 11 publications

References 51 publications

Infrared luminosity functions and dust mass functions in the EAGLE simulation

Infrared luminosity functions and dust mass functions in the EAGLE simulation

The molecular mass function of the local Universe

Modeling high-dimensional dependence in astronomical data

Contact Info

Product

Resources

About