(full page version here)
Research
Here is a link to all my publications registered in ADS : ADS publications
Below I detail some of the projects I have been spending time on during my PhD project and since then...
1. Cosmic web filaments in the CFHTLS
The importance of groups of galaxies and cosmic filaments in pre-processing the galaxy population before they enter galaxy clusters is not yet clear. The work soon to be submitted in Sarron
et al. (in prep), presented and reviewed by the jury in my PhD thesis manuscript focused on this aspect.
To detect cosmic filaments around AMASCFI clusters in the CFHTLS, we adapted the method proposed by Laigle et al.
(2018). The method consists in looking for filaments in the two-dimensional projected galaxy distribution in
redshift slices. The filament detection is done with DisPerSE (Sousbie 2011), a ridge finder algorithm.
Stay tuned for the results in the upcoming paper!
Reconstruction of the connected cosmic web filaments around a massive cluster the 100 deg2 EUCLID lightcone from Merson et al (2013). The reconstruction in a 2D slice using photometric redshift is shown in green, while the true 3D skeleton projected in the slice is shown in black. The filaments are detected using DisPerSE (Sousbie 2011). The red circle has a 1.5 cMpc radius.
2. A cluster finding algorithm : AMASCFI
I designed an algorithm called the Adami, MAzure and Sarron Cluster FInder (AMASCFI) to detect clusters of galaxies using large photometric surveys.
The main idea behind AMASCFI is to look for overdensities in overlapping redshift slices of the galaxy catalogue and then merge them into cluster candidates using a friend-of-friend algorithm. A mass estimate of the cluster candidates is derived a posterori using a scaling relation with the cluster richness.
The algorithm was built to handle large data sets such as Euclid or the Large Synoptic Survey Telescope (LSST), particularly using parallel programming on computer clusters.
I successfully applied AMASCFI to the full 154 deg2 of the CFHTLS in Sarron et al. (2018). We detected 7100 cluster candidates up to z = 1.1. The cluster candidate catalogue is publicly available on the VizieR portal.
Details on the AMASCFI algorithm, its selection function and the CFHTLS cluster candidate catalogue can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
I will do my best to publicly release AMASCFI (set of fortran routines) through github in the future...
Galaxy cluster detected by AMASCFI at a redshift z = 0.52
3. Cluster galaxy luminosity function in the CFHTLS
To study environmental galaxy quenching, we built the galaxy luminosity function (GLF) of AMASCFI cluster candidates (Sarron et al. 2018) for two galaxy populations: passive and star-forming. The segregation between the two populations was done using the photo-z code LePhare (Ilbert et al. 2006).
The size of our sample allowed us to explore jointly the redshift evolution and cluster mass dependence, thus breaking the degeneracy that exists between the two parameters for the first time.
Redshift evolution of the Schechter fit of early-type / passive (orange, red, and brown) and late-type / star-forming(green, light blue, and deep blue) galaxy luminosity function (GLF). The shaded areas are the 68% confidence interval on the fit. Adapated from Sarron et al. (2018)
The main result of our study is that the number of faint passive galaxies in clusters increases from redshift z = 0.7 to z = 0.1, the effect being slightly stronger in higher mass clusters. These results show that the red sequence is already in place at z > 0.7, and it keeps being enriched between these epochs through efficient environmental quenching (i.e. suppression of star-formation)
All the results can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
Contact
Address:
Centre de Biologie Intégrative
UNIV TOULOUSE PAUL SABATIER, 118 route de Narbonne
31062 Toulouse CEDEX 9
France
Email:
florian(.)sarron(at)irit(.)fr
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Preformatted
i = 0;
while (!deck.isInOrder()) {
print 'Iteration ' + i;
deck.shuffle();
i++;
}
print 'It took ' + i + ' iterations to sort the deck.';
Lists
Unordered
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Alternate
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Ordered
- Dolor pulvinar etiam.
- Etiam vel felis viverra.
- Felis enim feugiat.
- Dolor pulvinar etiam.
- Etiam vel felis lorem.
- Felis enim et feugiat.
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Actions
Table
Default
Name
Description
Price
Item One
Ante turpis integer aliquet porttitor.
29.99
Item Two
Vis ac commodo adipiscing arcu aliquet.
19.99
Item Three
Morbi faucibus arcu accumsan lorem.
29.99
Item Four
Vitae integer tempus condimentum.
19.99
Item Five
Ante turpis integer aliquet porttitor.
29.99
100.00
Alternate
Name
Description
Price
Item One
Ante turpis integer aliquet porttitor.
29.99
Item Two
Vis ac commodo adipiscing arcu aliquet.
19.99
Item Three
Morbi faucibus arcu accumsan lorem.
29.99
Item Four
Vitae integer tempus condimentum.
19.99
Item Five
Ante turpis integer aliquet porttitor.
29.99
100.00
Buttons
Form
The importance of groups of galaxies and cosmic filaments in pre-processing the galaxy population before they enter galaxy clusters is not yet clear. The work soon to be submitted in Sarron et al. (in prep), presented and reviewed by the jury in my PhD thesis manuscript focused on this aspect. To detect cosmic filaments around AMASCFI clusters in the CFHTLS, we adapted the method proposed by Laigle et al. (2018). The method consists in looking for filaments in the two-dimensional projected galaxy distribution in redshift slices. The filament detection is done with DisPerSE (Sousbie 2011), a ridge finder algorithm.
Stay tuned for the results in the upcoming paper!
Reconstruction of the connected cosmic web filaments around a massive cluster the 100 deg2 EUCLID lightcone from Merson et al (2013). The reconstruction in a 2D slice using photometric redshift is shown in green, while the true 3D skeleton projected in the slice is shown in black. The filaments are detected using DisPerSE (Sousbie 2011). The red circle has a 1.5 cMpc radius.2. A cluster finding algorithm : AMASCFI
I designed an algorithm called the Adami, MAzure and Sarron Cluster FInder (AMASCFI) to detect clusters of galaxies using large photometric surveys.
The main idea behind AMASCFI is to look for overdensities in overlapping redshift slices of the galaxy catalogue and then merge them into cluster candidates using a friend-of-friend algorithm. A mass estimate of the cluster candidates is derived a posterori using a scaling relation with the cluster richness.
The algorithm was built to handle large data sets such as Euclid or the Large Synoptic Survey Telescope (LSST), particularly using parallel programming on computer clusters.
I successfully applied AMASCFI to the full 154 deg2 of the CFHTLS in Sarron et al. (2018). We detected 7100 cluster candidates up to z = 1.1. The cluster candidate catalogue is publicly available on the VizieR portal.
Details on the AMASCFI algorithm, its selection function and the CFHTLS cluster candidate catalogue can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
I will do my best to publicly release AMASCFI (set of fortran routines) through github in the future...
Galaxy cluster detected by AMASCFI at a redshift z = 0.52
3. Cluster galaxy luminosity function in the CFHTLS
To study environmental galaxy quenching, we built the galaxy luminosity function (GLF) of AMASCFI cluster candidates (Sarron et al. 2018) for two galaxy populations: passive and star-forming. The segregation between the two populations was done using the photo-z code LePhare (Ilbert et al. 2006).
The size of our sample allowed us to explore jointly the redshift evolution and cluster mass dependence, thus breaking the degeneracy that exists between the two parameters for the first time.
Redshift evolution of the Schechter fit of early-type / passive (orange, red, and brown) and late-type / star-forming(green, light blue, and deep blue) galaxy luminosity function (GLF). The shaded areas are the 68% confidence interval on the fit. Adapated from Sarron et al. (2018)
The main result of our study is that the number of faint passive galaxies in clusters increases from redshift z = 0.7 to z = 0.1, the effect being slightly stronger in higher mass clusters. These results show that the red sequence is already in place at z > 0.7, and it keeps being enriched between these epochs through efficient environmental quenching (i.e. suppression of star-formation)
All the results can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
Contact
Address:
Centre de Biologie Intégrative
UNIV TOULOUSE PAUL SABATIER, 118 route de Narbonne
31062 Toulouse CEDEX 9
France
Email:
florian(.)sarron(at)irit(.)fr
Elements
Text
This is bold and this is strong. This is italic and this is emphasized.
This is superscript text and this is subscript text.
This is underlined and this is code: for (;;) { ... }
. Finally, this is a link.
Heading Level 2
Heading Level 3
Heading Level 4
Heading Level 5
Heading Level 6
Blockquote
Fringilla nisl. Donec accumsan interdum nisi, quis tincidunt felis sagittis eget tempus euismod. Vestibulum ante ipsum primis in faucibus vestibulum. Blandit adipiscing eu felis iaculis volutpat ac adipiscing accumsan faucibus. Vestibulum ante ipsum primis in faucibus lorem ipsum dolor sit amet nullam adipiscing eu felis.
Preformatted
i = 0;
while (!deck.isInOrder()) {
print 'Iteration ' + i;
deck.shuffle();
i++;
}
print 'It took ' + i + ' iterations to sort the deck.';
Lists
Unordered
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Alternate
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Ordered
- Dolor pulvinar etiam.
- Etiam vel felis viverra.
- Felis enim feugiat.
- Dolor pulvinar etiam.
- Etiam vel felis lorem.
- Felis enim et feugiat.
Icons
Actions
Table
Default
Name
Description
Price
Item One
Ante turpis integer aliquet porttitor.
29.99
Item Two
Vis ac commodo adipiscing arcu aliquet.
19.99
Item Three
Morbi faucibus arcu accumsan lorem.
29.99
Item Four
Vitae integer tempus condimentum.
19.99
Item Five
Ante turpis integer aliquet porttitor.
29.99
100.00
Alternate
Name
Description
Price
Item One
Ante turpis integer aliquet porttitor.
29.99
Item Two
Vis ac commodo adipiscing arcu aliquet.
19.99
Item Three
Morbi faucibus arcu accumsan lorem.
29.99
Item Four
Vitae integer tempus condimentum.
19.99
Item Five
Ante turpis integer aliquet porttitor.
29.99
100.00
Buttons
Form
I designed an algorithm called the Adami, MAzure and Sarron Cluster FInder (AMASCFI) to detect clusters of galaxies using large photometric surveys.
The main idea behind AMASCFI is to look for overdensities in overlapping redshift slices of the galaxy catalogue and then merge them into cluster candidates using a friend-of-friend algorithm. A mass estimate of the cluster candidates is derived a posterori using a scaling relation with the cluster richness.
The algorithm was built to handle large data sets such as Euclid or the Large Synoptic Survey Telescope (LSST), particularly using parallel programming on computer clusters.
I successfully applied AMASCFI to the full 154 deg2 of the CFHTLS in Sarron et al. (2018). We detected 7100 cluster candidates up to z = 1.1. The cluster candidate catalogue is publicly available on the VizieR portal.
Details on the AMASCFI algorithm, its selection function and the CFHTLS cluster candidate catalogue can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
I will do my best to publicly release AMASCFI (set of fortran routines) through github in the future...
Galaxy cluster detected by AMASCFI at a redshift z = 0.52 3. Cluster galaxy luminosity function in the CFHTLS
To study environmental galaxy quenching, we built the galaxy luminosity function (GLF) of AMASCFI cluster candidates (Sarron et al. 2018) for two galaxy populations: passive and star-forming. The segregation between the two populations was done using the photo-z code LePhare (Ilbert et al. 2006).
The size of our sample allowed us to explore jointly the redshift evolution and cluster mass dependence, thus breaking the degeneracy that exists between the two parameters for the first time.
Redshift evolution of the Schechter fit of early-type / passive (orange, red, and brown) and late-type / star-forming(green, light blue, and deep blue) galaxy luminosity function (GLF). The shaded areas are the 68% confidence interval on the fit. Adapated from Sarron et al. (2018)
The main result of our study is that the number of faint passive galaxies in clusters increases from redshift z = 0.7 to z = 0.1, the effect being slightly stronger in higher mass clusters. These results show that the red sequence is already in place at z > 0.7, and it keeps being enriched between these epochs through efficient environmental quenching (i.e. suppression of star-formation)
All the results can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
Contact
Address:
Centre de Biologie Intégrative
UNIV TOULOUSE PAUL SABATIER, 118 route de Narbonne
31062 Toulouse CEDEX 9
France
Email:
florian(.)sarron(at)irit(.)fr
Elements
Text
This is bold and this is strong. This is italic and this is emphasized.
This is superscript text and this is subscript text.
This is underlined and this is code: for (;;) { ... }
. Finally, this is a link.
Heading Level 2
Heading Level 3
Heading Level 4
Heading Level 5
Heading Level 6
Blockquote
Fringilla nisl. Donec accumsan interdum nisi, quis tincidunt felis sagittis eget tempus euismod. Vestibulum ante ipsum primis in faucibus vestibulum. Blandit adipiscing eu felis iaculis volutpat ac adipiscing accumsan faucibus. Vestibulum ante ipsum primis in faucibus lorem ipsum dolor sit amet nullam adipiscing eu felis.
Preformatted
i = 0;
while (!deck.isInOrder()) {
print 'Iteration ' + i;
deck.shuffle();
i++;
}
print 'It took ' + i + ' iterations to sort the deck.';
Lists
Unordered
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Alternate
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Ordered
- Dolor pulvinar etiam.
- Etiam vel felis viverra.
- Felis enim feugiat.
- Dolor pulvinar etiam.
- Etiam vel felis lorem.
- Felis enim et feugiat.
Icons
Actions
Table
Default
Name
Description
Price
Item One
Ante turpis integer aliquet porttitor.
29.99
Item Two
Vis ac commodo adipiscing arcu aliquet.
19.99
Item Three
Morbi faucibus arcu accumsan lorem.
29.99
Item Four
Vitae integer tempus condimentum.
19.99
Item Five
Ante turpis integer aliquet porttitor.
29.99
100.00
Alternate
Name
Description
Price
Item One
Ante turpis integer aliquet porttitor.
29.99
Item Two
Vis ac commodo adipiscing arcu aliquet.
19.99
Item Three
Morbi faucibus arcu accumsan lorem.
29.99
Item Four
Vitae integer tempus condimentum.
19.99
Item Five
Ante turpis integer aliquet porttitor.
29.99
100.00
Buttons
Form
To study environmental galaxy quenching, we built the galaxy luminosity function (GLF) of AMASCFI cluster candidates (Sarron et al. 2018) for two galaxy populations: passive and star-forming. The segregation between the two populations was done using the photo-z code LePhare (Ilbert et al. 2006).
The size of our sample allowed us to explore jointly the redshift evolution and cluster mass dependence, thus breaking the degeneracy that exists between the two parameters for the first time.
Redshift evolution of the Schechter fit of early-type / passive (orange, red, and brown) and late-type / star-forming(green, light blue, and deep blue) galaxy luminosity function (GLF). The shaded areas are the 68% confidence interval on the fit. Adapated from Sarron et al. (2018)The main result of our study is that the number of faint passive galaxies in clusters increases from redshift z = 0.7 to z = 0.1, the effect being slightly stronger in higher mass clusters. These results show that the red sequence is already in place at z > 0.7, and it keeps being enriched between these epochs through efficient environmental quenching (i.e. suppression of star-formation)
All the results can be found in Sarron, F., Martinet, N., Durret, F., et al. 2018, A&A, 613, A67
Contact
Centre de Biologie Intégrative
UNIV TOULOUSE PAUL SABATIER, 118 route de Narbonne
31062 Toulouse CEDEX 9
France
florian(.)sarron(at)irit(.)fr
Elements
Text
This is bold and this is strong. This is italic and this is emphasized.
This is superscript text and this is subscript text.
This is underlined and this is code: for (;;) { ... }
. Finally, this is a link.
Heading Level 2
Heading Level 3
Heading Level 4
Heading Level 5
Heading Level 6
Blockquote
Fringilla nisl. Donec accumsan interdum nisi, quis tincidunt felis sagittis eget tempus euismod. Vestibulum ante ipsum primis in faucibus vestibulum. Blandit adipiscing eu felis iaculis volutpat ac adipiscing accumsan faucibus. Vestibulum ante ipsum primis in faucibus lorem ipsum dolor sit amet nullam adipiscing eu felis.
Preformatted
i = 0;
while (!deck.isInOrder()) {
print 'Iteration ' + i;
deck.shuffle();
i++;
}
print 'It took ' + i + ' iterations to sort the deck.';
Lists
Unordered
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Alternate
- Dolor pulvinar etiam.
- Sagittis adipiscing.
- Felis enim feugiat.
Ordered
- Dolor pulvinar etiam.
- Etiam vel felis viverra.
- Felis enim feugiat.
- Dolor pulvinar etiam.
- Etiam vel felis lorem.
- Felis enim et feugiat.
Icons
Actions
Table
Default
Name | Description | Price |
---|---|---|
Item One | Ante turpis integer aliquet porttitor. | 29.99 |
Item Two | Vis ac commodo adipiscing arcu aliquet. | 19.99 |
Item Three | Morbi faucibus arcu accumsan lorem. | 29.99 |
Item Four | Vitae integer tempus condimentum. | 19.99 |
Item Five | Ante turpis integer aliquet porttitor. | 29.99 |
100.00 |
Alternate
Name | Description | Price |
---|---|---|
Item One | Ante turpis integer aliquet porttitor. | 29.99 |
Item Two | Vis ac commodo adipiscing arcu aliquet. | 19.99 |
Item Three | Morbi faucibus arcu accumsan lorem. | 29.99 |
Item Four | Vitae integer tempus condimentum. | 19.99 |
Item Five | Ante turpis integer aliquet porttitor. | 29.99 |
100.00 |