Darko Donevski | SISSA - Academia.edu (original) (raw)
Papers by Darko Donevski
The dataset contains the modelled gas-phase metallicities and gas masses based on SED-derived dus... more The dataset contains the modelled gas-phase metallicities and gas masses based on SED-derived dust and stellar properties for 300 ALMA detected dusty star-forming galaxies analysed in Donevski et al. A&A accepted, arXiv:2008.09995.
This talk is based on the work <em>Donevski et al. , to be submitted</em> - we aim to... more This talk is based on the work <em>Donevski et al. , to be submitted</em> - we aim to tackle one of existing challenges in dusty, galaxy formation and evolution by estimating the evolution of \(M_{\rm dust}/M_{\star}\)over cosmic time. I explain how to take particular care of understanding the eventual systematics of estimated physical properties. I show how we model and interpret our results in the context of galaxy formation and evolution by confronting the findings to the newest generation of galaxy models and simulations that include self-consistent dust growth. We find that the ratio between dust and stellar mass can be used as a great diagnostics to disentangle MS and SB galaxies over all redshifts.
Astronomy & Astrophysics, 2021
Aims. We study how the upcoming Legacy Survey of Space and Time (LSST) data from the Vera C. Rubi... more Aims. We study how the upcoming Legacy Survey of Space and Time (LSST) data from the Vera C. Rubin Observatory can be employed to constrain the physical properties of normal star-forming galaxies (main-sequence galaxies). Because the majority of the observed LSST objects will have no auxiliary data, we use simulated LSST data and existing real observations to test the reliability of estimates of the physical properties of galaxies, such as their star formation rate (SFR), stellar mass (Mstar), and dust luminosity (Ldust). We focus on normal star-forming galaxies because they form the majority of the galaxy population in the universe and are therefore more likely to be observed with the LSST. Methods. We performed a simulation of LSST observations and uncertainties of 50 385 real galaxies within the redshift range 0
Astronomy & Astrophysics, 2018
Context. Over the last decade a large number of dusty star-forming galaxies has been discovered u... more Context. Over the last decade a large number of dusty star-forming galaxies has been discovered up to redshift z = 2 − 3 and recent studies have attempted to push the highly confused Herschel SPIRE surveys beyond that distance. To search for z ≥ 4 galaxies they often consider the sources with fluxes rising from 250 μm to 500 μm (so-called “500 μm-risers”). Herschel surveys offer a unique opportunity to efficiently select a large number of these rare objects, and thus gain insight into the prodigious star-forming activity that takes place in the very distant Universe. Aims. We aim to implement a novel method to obtain a statistical sample of 500 μm-risers and fully evaluate our selection inspecting different models of galaxy evolution. Methods. We consider one of the largest and deepest Herschel surveys, the Herschel Virgo Cluster Survey. We develop a novel selection algorithm which links the source extraction and spectral energy distribution fitting. To fully quantify selection bias...
Monthly Notices of the Royal Astronomical Society, 2015
Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum... more Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum radio and dust emission of star-forming galaxies, often used as a tool in determining star formation rates. Here we expand the point made by Murphy that in the case of some interacting star-forming galaxies there is a non-thermal emission from the gas bridge in between them, which might cause a dispersion in this correlation. Galactic interactions and mergers have been known to give rise to tidal shocks and disrupt morphologies especially in the smaller of the interacting components. Here we point out that these shocks can also heat the gas and dust and will inevitably accelerate particles and result in a tidal cosmic ray population in addition to standard galactic cosmic rays in the galaxy itself. This would result in a non-thermal emission not only from the gas bridges of interacting systems, but from interacting galaxies as a whole in general. Thus both tidal heating and additional non-thermal radiation will obviously affect the FIR-radio correlation of these systems, the only question is how much. In this scenario the FIR-radio correlation is not stable in interacting galaxies, but rather evolves as the interaction/merger progresses. To test this hypothesis and probe the possible impact of tidal cosmic ray population, we have analysed a sample of 43 infrared-bright star-forming interacting galaxies at different merger stages. We have found that their FIR-radio correlation parameter and radio emission spectral index vary noticeably over different merger stages and behave as it would be expected from our tidal-shock scenario. Important implications of departure of interacting galaxies from the FIR-radio correlation are discussed.
Far-infrared (FIR)--radio correlation is a well-established empirical connection between continuu... more Far-infrared (FIR)--radio correlation is a well-established empirical connection between continuum radio and dust emission of star-forming galaxies, used as a tool in determining star-formation rates. Here we point out that in the case of interacting star-forming galaxies this tool might break. Galactic interactions and mergers have been known to give rise to tidal shocks and disrupt morphologies especially in the smaller of the interacting components. Moreover, these shocks can also heat the gas and dust and accelerate particles leading to tidal cosmic-ray population in addition to standard galactic cosmic rays. Both heating and additional non-thermal radiation will obviously affect the FIR-radio correlation of these systems. To test this hypothesis we have analyzed a sample of 43 infrared bright star-forming interacting galaxies at different merger stages. We have found that their FIR-radio correlation parameter and radio emission spectral index vary over different merger stages a...
The Astrophysical Journal, 2021
In this paper, we study the impact of different galaxy statistics and empirical metallicity scali... more In this paper, we study the impact of different galaxy statistics and empirical metallicity scaling relations on the merging rates and properties of compact object binaries. Firstly, we analyze the similarities and differences of using the star formation rate functions versus stellar mass functions as galaxy statistics for the computation of cosmic star formation rate density. We then investigate the effects of adopting the Fundamental Metallicity Relation versus a classic Mass Metallicity Relation to assign metallicity to galaxies with given properties. We find that when the Fundamental Metallicity Relation is exploited, the bulk of the star formation occurs at relatively high metallicities, even at high redshift; the opposite holds when the Mass Metallicity Relation is employed, since in this case the metallicity at which most of the star formation takes place strongly decreases with redshift. We discuss the various reasons and possible biases giving rise to this discrepancy. Fina...
The Astrophysical Journal
We have obtained three-dimensional maps of the universe in ∼ 200×200×80 comoving Mpc 3 (cMpc 3) v... more We have obtained three-dimensional maps of the universe in ∼ 200×200×80 comoving Mpc 3 (cMpc 3) volumes each at z = 5.7 and 6.6 based on a spectroscopic sample of 179 galaxies that achieves 80% completeness down to the Lyα luminosity of log(L Lyα /[erg s −1 ]) = 43.0, based on our Keck and Gemini observations and the literature. The maps reveal filamentary large-scale structures and two remarkable overdensities made out of at least 44 and 12 galaxies at z = 5.692 (z57OD) and z = 6.585 (z66OD), respectively, making z66OD the most distant overdensity spectroscopically confirmed to date with > 10 spectroscopically confirmed galaxies. We compare spatial distributions of submillimeter galaxies at z 4 − 6 with our z = 5.7 galaxies forming the large-scale structures, and detect a 99.97% signal of cross correlation, indicative of a clear coincidence of dusty star-forming galaxy and dust unobscured galaxy formation at this early epoch. The galaxies in z57OD and z66OD are actively forming stars with star formation rates (SFRs) 5 times higher than the main sequence, and particularly the SFR density in z57OD is 10 times higher than the cosmic average at the redshift (a.k.a. the Madau-Lilly plot). Comparisons with numerical simulations suggest that z57OD and z66OD are protoclusters that are progenitors of the present-day clusters with halo masses of ∼ 10 14 M .
Context. Over the last decade a large number of dusty star forming galaxies has been discovered u... more Context. Over the last decade a large number of dusty star forming galaxies has been discovered up to redshift z = 2 − 3 and recent studies have attempted to push the highly-confused Herschel SPIRE surveys beyond that distance. To search for z ≥ 4 galaxies they often consider the sources with fluxes rising from 250 µm to 500 µm (so-called "500 µm-risers"). Herschel surveys offer a unique opportunity to efficiently select a large number of these rare objects, and thus gain insight into the prodigious star-forming activity that takes place in the very distant Universe. Aims. We aim to implement a novel method to obtain a statistical sample of "500 µm-risers" and fully evaluate our selection inspecting different models of galaxy evolution. Methods. We consider one of the largest and deepest Herschel surveys, the Herschel Virgo Cluster Survey. We develop a novel selection algorithm which links the source extraction and spectral energy distribution fitting. To fully quantify selection biases we make end-to-end simulations including clustering and lensing. Results. We select 133 "500 µm-risers" over 55 deg 2 , imposing the criteria: S 500 > S 350 > S 250 , S 250 > 13.2 mJy and S 500 > 30 mJy. Differential number counts are in a fairly good agreement with models, displaying better match than other existing samples. The estimated fraction of strongly lensed sources is 24 +6 −5 % based on models. Conclusions. We present the faintest sample of "500 µm-risers" down to S 250 = 13.2 mJy. We show that noise and weak lensing have an important impact on measured counts and redshift distribution of selected sources. We estimate the flux-corrected star formation rate density at 4 < z < 5 with the "500 µm-risers" and found it close to the total value measured in far-infrared. It indicates that colour selection is not a limiting effect to search for the most massive, dusty z > 4 sources.
Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum... more Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum radio and dust emission of star-forming galaxies, often used as a tool in determining star formation rates. Here we expand the point made by Murphy that in the case of some interacting star-forming galaxies there is a non-thermal emission from the gas bridge in between them, which might cause a dispersion in this correlation. Galactic interactions and mergers have been known to give rise to tidal shocks and disrupt morphologies especially in the smaller of the interacting components. Here we point out that these shocks can also heat the gas and dust and will inevitably accelerate particles and result in a tidal cosmic ray population in addition to standard galactic cosmic rays in the galaxy itself. This would result in a non-thermal emission not only from the gas bridges of interacting systems, but from interacting galaxies as a whole in general. Thus both tidal heating and additional non-thermal radiation will obviously affect the FIR-radio correlation of these systems, the only question is how much. In this scenario the FIR-radio correlation is not stable in interacting galaxies, but rather evolves as the interaction/merger progresses. To test this hypothesis and probe the possible impact of tidal cosmic ray population, we have analysed a sample of 43 infrared-bright star-forming interacting galaxies at different merger stages. We have found that their FIR-radio correlation parameter and radio emission spectral index vary noticeably over different merger stages and behave as it would be expected from our tidal-shock scenario. Important implications of departure of interacting galaxies from the FIR-radio correlation are discussed.
DESCRIPTION It is known that close galactic fly-bys and interactions give rise to shock waves tha... more DESCRIPTION It is known that close galactic fly-bys and interactions give rise to shock waves that disrupt the interstellar medium of galaxies and impact their morphologies. These large-scale shocks that form in the interstellar medium of interacting systems will be the sites of particle acceleration giving rise to a population of tidal cosmic rays, in addition to standard galactic cosmic rays present in star-forming galaxies.
Supernova explosions release burst of neutrinos. We explore following process that those neutrino... more Supernova explosions release burst of neutrinos. We explore following process that those neutrinos induce in hydrogen-rich environments: (proton+electron antineutrino = neutron +positron) in order to get an "early" direction and energy released in a nearby future hypernova explosion. Neutron captures onto proton while positron annihilates, which results in production of gamma rays of energy 2.22 and 0.511 MeV, respectively. Our idea is to use Sun to detect this kind of events early (before optical observatories) based on the neutrino-induced solar gamma rays expected from a hypernova with a 100 solar mass progenitor, like Eta Carinae for example. Hypernovae are characterized by explosion energies larger than 10^52 erg. This is basically a theoretical assessment of gamma ray flux which is induced in surface layer of the Sun, due to interaction with neutrinos which were emmited during explosion of a nearby hypernova. We will also try to investrigate possible model for probin...
The dataset contains the modelled gas-phase metallicities and gas masses based on SED-derived dus... more The dataset contains the modelled gas-phase metallicities and gas masses based on SED-derived dust and stellar properties for 300 ALMA detected dusty star-forming galaxies analysed in Donevski et al. A&A accepted, arXiv:2008.09995.
This talk is based on the work <em>Donevski et al. , to be submitted</em> - we aim to... more This talk is based on the work <em>Donevski et al. , to be submitted</em> - we aim to tackle one of existing challenges in dusty, galaxy formation and evolution by estimating the evolution of \(M_{\rm dust}/M_{\star}\)over cosmic time. I explain how to take particular care of understanding the eventual systematics of estimated physical properties. I show how we model and interpret our results in the context of galaxy formation and evolution by confronting the findings to the newest generation of galaxy models and simulations that include self-consistent dust growth. We find that the ratio between dust and stellar mass can be used as a great diagnostics to disentangle MS and SB galaxies over all redshifts.
Astronomy & Astrophysics, 2021
Aims. We study how the upcoming Legacy Survey of Space and Time (LSST) data from the Vera C. Rubi... more Aims. We study how the upcoming Legacy Survey of Space and Time (LSST) data from the Vera C. Rubin Observatory can be employed to constrain the physical properties of normal star-forming galaxies (main-sequence galaxies). Because the majority of the observed LSST objects will have no auxiliary data, we use simulated LSST data and existing real observations to test the reliability of estimates of the physical properties of galaxies, such as their star formation rate (SFR), stellar mass (Mstar), and dust luminosity (Ldust). We focus on normal star-forming galaxies because they form the majority of the galaxy population in the universe and are therefore more likely to be observed with the LSST. Methods. We performed a simulation of LSST observations and uncertainties of 50 385 real galaxies within the redshift range 0
Astronomy & Astrophysics, 2018
Context. Over the last decade a large number of dusty star-forming galaxies has been discovered u... more Context. Over the last decade a large number of dusty star-forming galaxies has been discovered up to redshift z = 2 − 3 and recent studies have attempted to push the highly confused Herschel SPIRE surveys beyond that distance. To search for z ≥ 4 galaxies they often consider the sources with fluxes rising from 250 μm to 500 μm (so-called “500 μm-risers”). Herschel surveys offer a unique opportunity to efficiently select a large number of these rare objects, and thus gain insight into the prodigious star-forming activity that takes place in the very distant Universe. Aims. We aim to implement a novel method to obtain a statistical sample of 500 μm-risers and fully evaluate our selection inspecting different models of galaxy evolution. Methods. We consider one of the largest and deepest Herschel surveys, the Herschel Virgo Cluster Survey. We develop a novel selection algorithm which links the source extraction and spectral energy distribution fitting. To fully quantify selection bias...
Monthly Notices of the Royal Astronomical Society, 2015
Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum... more Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum radio and dust emission of star-forming galaxies, often used as a tool in determining star formation rates. Here we expand the point made by Murphy that in the case of some interacting star-forming galaxies there is a non-thermal emission from the gas bridge in between them, which might cause a dispersion in this correlation. Galactic interactions and mergers have been known to give rise to tidal shocks and disrupt morphologies especially in the smaller of the interacting components. Here we point out that these shocks can also heat the gas and dust and will inevitably accelerate particles and result in a tidal cosmic ray population in addition to standard galactic cosmic rays in the galaxy itself. This would result in a non-thermal emission not only from the gas bridges of interacting systems, but from interacting galaxies as a whole in general. Thus both tidal heating and additional non-thermal radiation will obviously affect the FIR-radio correlation of these systems, the only question is how much. In this scenario the FIR-radio correlation is not stable in interacting galaxies, but rather evolves as the interaction/merger progresses. To test this hypothesis and probe the possible impact of tidal cosmic ray population, we have analysed a sample of 43 infrared-bright star-forming interacting galaxies at different merger stages. We have found that their FIR-radio correlation parameter and radio emission spectral index vary noticeably over different merger stages and behave as it would be expected from our tidal-shock scenario. Important implications of departure of interacting galaxies from the FIR-radio correlation are discussed.
Far-infrared (FIR)--radio correlation is a well-established empirical connection between continuu... more Far-infrared (FIR)--radio correlation is a well-established empirical connection between continuum radio and dust emission of star-forming galaxies, used as a tool in determining star-formation rates. Here we point out that in the case of interacting star-forming galaxies this tool might break. Galactic interactions and mergers have been known to give rise to tidal shocks and disrupt morphologies especially in the smaller of the interacting components. Moreover, these shocks can also heat the gas and dust and accelerate particles leading to tidal cosmic-ray population in addition to standard galactic cosmic rays. Both heating and additional non-thermal radiation will obviously affect the FIR-radio correlation of these systems. To test this hypothesis we have analyzed a sample of 43 infrared bright star-forming interacting galaxies at different merger stages. We have found that their FIR-radio correlation parameter and radio emission spectral index vary over different merger stages a...
The Astrophysical Journal, 2021
In this paper, we study the impact of different galaxy statistics and empirical metallicity scali... more In this paper, we study the impact of different galaxy statistics and empirical metallicity scaling relations on the merging rates and properties of compact object binaries. Firstly, we analyze the similarities and differences of using the star formation rate functions versus stellar mass functions as galaxy statistics for the computation of cosmic star formation rate density. We then investigate the effects of adopting the Fundamental Metallicity Relation versus a classic Mass Metallicity Relation to assign metallicity to galaxies with given properties. We find that when the Fundamental Metallicity Relation is exploited, the bulk of the star formation occurs at relatively high metallicities, even at high redshift; the opposite holds when the Mass Metallicity Relation is employed, since in this case the metallicity at which most of the star formation takes place strongly decreases with redshift. We discuss the various reasons and possible biases giving rise to this discrepancy. Fina...
The Astrophysical Journal
We have obtained three-dimensional maps of the universe in ∼ 200×200×80 comoving Mpc 3 (cMpc 3) v... more We have obtained three-dimensional maps of the universe in ∼ 200×200×80 comoving Mpc 3 (cMpc 3) volumes each at z = 5.7 and 6.6 based on a spectroscopic sample of 179 galaxies that achieves 80% completeness down to the Lyα luminosity of log(L Lyα /[erg s −1 ]) = 43.0, based on our Keck and Gemini observations and the literature. The maps reveal filamentary large-scale structures and two remarkable overdensities made out of at least 44 and 12 galaxies at z = 5.692 (z57OD) and z = 6.585 (z66OD), respectively, making z66OD the most distant overdensity spectroscopically confirmed to date with > 10 spectroscopically confirmed galaxies. We compare spatial distributions of submillimeter galaxies at z 4 − 6 with our z = 5.7 galaxies forming the large-scale structures, and detect a 99.97% signal of cross correlation, indicative of a clear coincidence of dusty star-forming galaxy and dust unobscured galaxy formation at this early epoch. The galaxies in z57OD and z66OD are actively forming stars with star formation rates (SFRs) 5 times higher than the main sequence, and particularly the SFR density in z57OD is 10 times higher than the cosmic average at the redshift (a.k.a. the Madau-Lilly plot). Comparisons with numerical simulations suggest that z57OD and z66OD are protoclusters that are progenitors of the present-day clusters with halo masses of ∼ 10 14 M .
Context. Over the last decade a large number of dusty star forming galaxies has been discovered u... more Context. Over the last decade a large number of dusty star forming galaxies has been discovered up to redshift z = 2 − 3 and recent studies have attempted to push the highly-confused Herschel SPIRE surveys beyond that distance. To search for z ≥ 4 galaxies they often consider the sources with fluxes rising from 250 µm to 500 µm (so-called "500 µm-risers"). Herschel surveys offer a unique opportunity to efficiently select a large number of these rare objects, and thus gain insight into the prodigious star-forming activity that takes place in the very distant Universe. Aims. We aim to implement a novel method to obtain a statistical sample of "500 µm-risers" and fully evaluate our selection inspecting different models of galaxy evolution. Methods. We consider one of the largest and deepest Herschel surveys, the Herschel Virgo Cluster Survey. We develop a novel selection algorithm which links the source extraction and spectral energy distribution fitting. To fully quantify selection biases we make end-to-end simulations including clustering and lensing. Results. We select 133 "500 µm-risers" over 55 deg 2 , imposing the criteria: S 500 > S 350 > S 250 , S 250 > 13.2 mJy and S 500 > 30 mJy. Differential number counts are in a fairly good agreement with models, displaying better match than other existing samples. The estimated fraction of strongly lensed sources is 24 +6 −5 % based on models. Conclusions. We present the faintest sample of "500 µm-risers" down to S 250 = 13.2 mJy. We show that noise and weak lensing have an important impact on measured counts and redshift distribution of selected sources. We estimate the flux-corrected star formation rate density at 4 < z < 5 with the "500 µm-risers" and found it close to the total value measured in far-infrared. It indicates that colour selection is not a limiting effect to search for the most massive, dusty z > 4 sources.
Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum... more Far-infrared (FIR)-radio correlation is a well-established empirical connection between continuum radio and dust emission of star-forming galaxies, often used as a tool in determining star formation rates. Here we expand the point made by Murphy that in the case of some interacting star-forming galaxies there is a non-thermal emission from the gas bridge in between them, which might cause a dispersion in this correlation. Galactic interactions and mergers have been known to give rise to tidal shocks and disrupt morphologies especially in the smaller of the interacting components. Here we point out that these shocks can also heat the gas and dust and will inevitably accelerate particles and result in a tidal cosmic ray population in addition to standard galactic cosmic rays in the galaxy itself. This would result in a non-thermal emission not only from the gas bridges of interacting systems, but from interacting galaxies as a whole in general. Thus both tidal heating and additional non-thermal radiation will obviously affect the FIR-radio correlation of these systems, the only question is how much. In this scenario the FIR-radio correlation is not stable in interacting galaxies, but rather evolves as the interaction/merger progresses. To test this hypothesis and probe the possible impact of tidal cosmic ray population, we have analysed a sample of 43 infrared-bright star-forming interacting galaxies at different merger stages. We have found that their FIR-radio correlation parameter and radio emission spectral index vary noticeably over different merger stages and behave as it would be expected from our tidal-shock scenario. Important implications of departure of interacting galaxies from the FIR-radio correlation are discussed.
DESCRIPTION It is known that close galactic fly-bys and interactions give rise to shock waves tha... more DESCRIPTION It is known that close galactic fly-bys and interactions give rise to shock waves that disrupt the interstellar medium of galaxies and impact their morphologies. These large-scale shocks that form in the interstellar medium of interacting systems will be the sites of particle acceleration giving rise to a population of tidal cosmic rays, in addition to standard galactic cosmic rays present in star-forming galaxies.
Supernova explosions release burst of neutrinos. We explore following process that those neutrino... more Supernova explosions release burst of neutrinos. We explore following process that those neutrinos induce in hydrogen-rich environments: (proton+electron antineutrino = neutron +positron) in order to get an "early" direction and energy released in a nearby future hypernova explosion. Neutron captures onto proton while positron annihilates, which results in production of gamma rays of energy 2.22 and 0.511 MeV, respectively. Our idea is to use Sun to detect this kind of events early (before optical observatories) based on the neutrino-induced solar gamma rays expected from a hypernova with a 100 solar mass progenitor, like Eta Carinae for example. Hypernovae are characterized by explosion energies larger than 10^52 erg. This is basically a theoretical assessment of gamma ray flux which is induced in surface layer of the Sun, due to interaction with neutrinos which were emmited during explosion of a nearby hypernova. We will also try to investrigate possible model for probin...