Andrea Botteon
@andreabotteon.bsky.social
Astrophysicist at INAF-IRA. Previously at UniBologna and UniLeiden. Mainly dealing with colliding galaxy clusters, merger shocks and their radio outcome.
Check for the wonderful science that @axisprobe.bsky.social would enable in the white book uploaded today in arXiv: arxiv.org/abs/2511.00253
I've participated with a chapter on "X-ray and radio surface brightness edges in the ICM", you can find it in the Galaxies GO Science section (page 69)
I've participated with a chapter on "X-ray and radio surface brightness edges in the ICM", you can find it in the Galaxies GO Science section (page 69)
November 4, 2025 at 8:47 AM
Check for the wonderful science that @axisprobe.bsky.social would enable in the white book uploaded today in arXiv: arxiv.org/abs/2511.00253
I've participated with a chapter on "X-ray and radio surface brightness edges in the ICM", you can find it in the Galaxies GO Science section (page 69)
I've participated with a chapter on "X-ray and radio surface brightness edges in the ICM", you can find it in the Galaxies GO Science section (page 69)
News on Abell 754 from @XRISM_jp, by Okabe+ and Omiya+
Combining the gas kinematic from XRISM and WL from Subauru, a new merger scenario is proposed. The "3rd dimension" has been unlocked thanks to XRISM 😀
arxiv.org/abs/2510.16291
arxiv.org/abs/2510.16553
Combining the gas kinematic from XRISM and WL from Subauru, a new merger scenario is proposed. The "3rd dimension" has been unlocked thanks to XRISM 😀
arxiv.org/abs/2510.16291
arxiv.org/abs/2510.16553
October 21, 2025 at 7:54 AM
News on Abell 754 from @XRISM_jp, by Okabe+ and Omiya+
Combining the gas kinematic from XRISM and WL from Subauru, a new merger scenario is proposed. The "3rd dimension" has been unlocked thanks to XRISM 😀
arxiv.org/abs/2510.16291
arxiv.org/abs/2510.16553
Combining the gas kinematic from XRISM and WL from Subauru, a new merger scenario is proposed. The "3rd dimension" has been unlocked thanks to XRISM 😀
arxiv.org/abs/2510.16291
arxiv.org/abs/2510.16553
The radio emission nicely follows the elongation of the X-ray emission from the clusters and intra-cluster bridge, suggesting that it is likely generated as consequence of the cluster-cluster encounter. In-between the clusters, the radio emission is enhanced 4/7
September 19, 2025 at 3:56 AM
The radio emission nicely follows the elongation of the X-ray emission from the clusters and intra-cluster bridge, suggesting that it is likely generated as consequence of the cluster-cluster encounter. In-between the clusters, the radio emission is enhanced 4/7
After careful analysis and removal of discrete sources, we confirmed the presence of the extended emission. The large-FoV images show that diffuse emission is present only at the position of the cluster pair in the MeerKAT field, while we have a non-detection with the uGMRT 3/7
September 19, 2025 at 3:56 AM
After careful analysis and removal of discrete sources, we confirmed the presence of the extended emission. The large-FoV images show that diffuse emission is present only at the position of the cluster pair in the MeerKAT field, while we have a non-detection with the uGMRT 3/7
The clusters are interacting and are likely observed shortly after pericenter passage. From the MeerKAT images, we noticed "excess" diffuse emission in the intra-cluster region 2/7
September 19, 2025 at 3:56 AM
The clusters are interacting and are likely observed shortly after pericenter passage. From the MeerKAT images, we noticed "excess" diffuse emission in the intra-cluster region 2/7
New paper alert! We studied a galaxy cluster pair with @SKA_Africa MeerKAT UHF and @NCRA_Outreach uGMRT band 3 data and found diffuse emission between the two clusters! 1/7
arxiv.org/abs/2509.14348
arxiv.org/abs/2509.14348
September 19, 2025 at 3:56 AM
New paper alert! We studied a galaxy cluster pair with @SKA_Africa MeerKAT UHF and @NCRA_Outreach uGMRT band 3 data and found diffuse emission between the two clusters! 1/7
arxiv.org/abs/2509.14348
arxiv.org/abs/2509.14348
Where is the counter lobe? An interesting hypothesis is that it could have been stretched as a consequence of the sloshing in the system, resulting in what is now observed as bridge/arc. See also our recent MeerKAT paper on Ophiuchus (arxiv.org/abs/2504.16158)!
August 29, 2025 at 7:19 AM
Where is the counter lobe? An interesting hypothesis is that it could have been stretched as a consequence of the sloshing in the system, resulting in what is now observed as bridge/arc. See also our recent MeerKAT paper on Ophiuchus (arxiv.org/abs/2504.16158)!
Low frequency observations of the Ophiuchus cluster, by Giacintucci+
The giant fossil lobe is studied in detail. The new data show steep spectrum filamentary structures embedded in the lobe. The lobe extends up to 820 kpc from the cluster center
arxiv.org/abs/2508.20190
The giant fossil lobe is studied in detail. The new data show steep spectrum filamentary structures embedded in the lobe. The lobe extends up to 820 kpc from the cluster center
arxiv.org/abs/2508.20190
August 29, 2025 at 7:19 AM
Low frequency observations of the Ophiuchus cluster, by Giacintucci+
The giant fossil lobe is studied in detail. The new data show steep spectrum filamentary structures embedded in the lobe. The lobe extends up to 820 kpc from the cluster center
arxiv.org/abs/2508.20190
The giant fossil lobe is studied in detail. The new data show steep spectrum filamentary structures embedded in the lobe. The lobe extends up to 820 kpc from the cluster center
arxiv.org/abs/2508.20190
.@XRISM_jp obs of the Ophiuchus cluster, by Fujita+
A low velocity dispersion is measured in the inner and outer regions (115 km/s at <25kpc, 186 km/s at 25-50 kpc). The same goes for the bulk velocity (8 km/s vs 104 km/s): is the sloshing at its minimum?
arxiv.org/abs/2507.00126
A low velocity dispersion is measured in the inner and outer regions (115 km/s at <25kpc, 186 km/s at 25-50 kpc). The same goes for the bulk velocity (8 km/s vs 104 km/s): is the sloshing at its minimum?
arxiv.org/abs/2507.00126
July 2, 2025 at 6:45 AM
.@XRISM_jp obs of the Ophiuchus cluster, by Fujita+
A low velocity dispersion is measured in the inner and outer regions (115 km/s at <25kpc, 186 km/s at 25-50 kpc). The same goes for the bulk velocity (8 km/s vs 104 km/s): is the sloshing at its minimum?
arxiv.org/abs/2507.00126
A low velocity dispersion is measured in the inner and outer regions (115 km/s at <25kpc, 186 km/s at 25-50 kpc). The same goes for the bulk velocity (8 km/s vs 104 km/s): is the sloshing at its minimum?
arxiv.org/abs/2507.00126
The magnetic field in A2142, by Pagliotta+
A rotation measure and polarization study is performed with MeerKAT. The magnetic field profile of the ICM is drawn, indicating a central field strength of 9.5 muG at the cluster center.
arxiv.org/abs/2507.00114
A rotation measure and polarization study is performed with MeerKAT. The magnetic field profile of the ICM is drawn, indicating a central field strength of 9.5 muG at the cluster center.
arxiv.org/abs/2507.00114
July 2, 2025 at 6:36 AM
The magnetic field in A2142, by Pagliotta+
A rotation measure and polarization study is performed with MeerKAT. The magnetic field profile of the ICM is drawn, indicating a central field strength of 9.5 muG at the cluster center.
arxiv.org/abs/2507.00114
A rotation measure and polarization study is performed with MeerKAT. The magnetic field profile of the ICM is drawn, indicating a central field strength of 9.5 muG at the cluster center.
arxiv.org/abs/2507.00114
MeerKAT observations of CHEX-MATE clusters, by Balboni+ (w/ @annalisa-astro.bsky.social, myself++)
A sample of 21 massive clusters is studied. Diffuse radio emission is detected in all systems (new halos and relics!)
arxiv.org/abs/2507.00133
A sample of 21 massive clusters is studied. Diffuse radio emission is detected in all systems (new halos and relics!)
arxiv.org/abs/2507.00133
July 2, 2025 at 6:33 AM
MeerKAT observations of CHEX-MATE clusters, by Balboni+ (w/ @annalisa-astro.bsky.social, myself++)
A sample of 21 massive clusters is studied. Diffuse radio emission is detected in all systems (new halos and relics!)
arxiv.org/abs/2507.00133
A sample of 21 massive clusters is studied. Diffuse radio emission is detected in all systems (new halos and relics!)
arxiv.org/abs/2507.00133
The central region of A3667 in hard X-rays, by @MSMirakhor+@astroswalker
A @NASANuSTAR observation of the cluster is presented. The spectrum is better described by a 2T thermal model. An updated limit of B > 0.2 muG is provided from the lack of IC emission
arxiv.org/abs/2505.20453
A @NASANuSTAR observation of the cluster is presented. The spectrum is better described by a 2T thermal model. An updated limit of B > 0.2 muG is provided from the lack of IC emission
arxiv.org/abs/2505.20453
May 28, 2025 at 6:12 AM
The central region of A3667 in hard X-rays, by @MSMirakhor+@astroswalker
A @NASANuSTAR observation of the cluster is presented. The spectrum is better described by a 2T thermal model. An updated limit of B > 0.2 muG is provided from the lack of IC emission
arxiv.org/abs/2505.20453
A @NASANuSTAR observation of the cluster is presented. The spectrum is better described by a 2T thermal model. An updated limit of B > 0.2 muG is provided from the lack of IC emission
arxiv.org/abs/2505.20453
Thin filaments in the tails of A2255, by DeRubeis+ (w/ myself, @jurjen93.bsky.social+)
A2255 is known to be a "mess" (arxiv.org/abs/2006.04808). The new @LOFAR-VLBI images add further complexity in the system, this time revealing small-scale structures in its radio galaxies
arxiv.org/abs/2505.13595
A2255 is known to be a "mess" (arxiv.org/abs/2006.04808). The new @LOFAR-VLBI images add further complexity in the system, this time revealing small-scale structures in its radio galaxies
arxiv.org/abs/2505.13595
May 21, 2025 at 6:17 AM
Thin filaments in the tails of A2255, by DeRubeis+ (w/ myself, @jurjen93.bsky.social+)
A2255 is known to be a "mess" (arxiv.org/abs/2006.04808). The new @LOFAR-VLBI images add further complexity in the system, this time revealing small-scale structures in its radio galaxies
arxiv.org/abs/2505.13595
A2255 is known to be a "mess" (arxiv.org/abs/2006.04808). The new @LOFAR-VLBI images add further complexity in the system, this time revealing small-scale structures in its radio galaxies
arxiv.org/abs/2505.13595
We pointed out how a second "outer component" of the halo surface brightness profile can arise when an improper source subtraction/masking is performed. Also the sector choice is critical, as different geometries, directions, and centers can generate the second component
3/4
3/4
May 9, 2025 at 6:54 AM
We pointed out how a second "outer component" of the halo surface brightness profile can arise when an improper source subtraction/masking is performed. Also the sector choice is critical, as different geometries, directions, and centers can generate the second component
3/4
3/4
These halos follow a single exponential profile in surface brightness, despite their large extents and complex dynamical state, and have emissivities similar to those of the other halos known. These massive clusters were good candidates to hosts the so-called mega halos
2/4
2/4
May 9, 2025 at 6:54 AM
These halos follow a single exponential profile in surface brightness, despite their large extents and complex dynamical state, and have emissivities similar to those of the other halos known. These massive clusters were good candidates to hosts the so-called mega halos
2/4
2/4
Radial properties of radio halos, by Rajpurohit+ (w/ myself+)
New radio halos with LLS>2 Mpc are reported, even at high-frequency. We measured the surface brightness and spectral properties of the emission, obtaining important results (more below)
arxiv.org/abs/2505.05415
1/4
New radio halos with LLS>2 Mpc are reported, even at high-frequency. We measured the surface brightness and spectral properties of the emission, obtaining important results (more below)
arxiv.org/abs/2505.05415
1/4
May 9, 2025 at 6:54 AM
Radial properties of radio halos, by Rajpurohit+ (w/ myself+)
New radio halos with LLS>2 Mpc are reported, even at high-frequency. We measured the surface brightness and spectral properties of the emission, obtaining important results (more below)
arxiv.org/abs/2505.05415
1/4
New radio halos with LLS>2 Mpc are reported, even at high-frequency. We measured the surface brightness and spectral properties of the emission, obtaining important results (more below)
arxiv.org/abs/2505.05415
1/4
Measurements of gas velocities in the ICM in the Coma cluster by @XRISM_jp
This is the first time that the gas velocity dispersion is measured in a merging cluster with a microcalorimeter! Interesting results: sigma_v is low while v_bulk is quite high...
arxiv.org/abs/2504.20928
This is the first time that the gas velocity dispersion is measured in a merging cluster with a microcalorimeter! Interesting results: sigma_v is low while v_bulk is quite high...
arxiv.org/abs/2504.20928
April 30, 2025 at 7:18 AM
Measurements of gas velocities in the ICM in the Coma cluster by @XRISM_jp
This is the first time that the gas velocity dispersion is measured in a merging cluster with a microcalorimeter! Interesting results: sigma_v is low while v_bulk is quite high...
arxiv.org/abs/2504.20928
This is the first time that the gas velocity dispersion is measured in a merging cluster with a microcalorimeter! Interesting results: sigma_v is low while v_bulk is quite high...
arxiv.org/abs/2504.20928
Finally, we reinterpret the amorphous radio source previously classified as a radio phoenix as a radio galaxy whose jet is undergoing kink instability. This scenario is supported by recent MHD simulations of unstable jets that show remarkable similar features (e.g. the ribs)
7/8
7/8
April 24, 2025 at 6:25 AM
Finally, we reinterpret the amorphous radio source previously classified as a radio phoenix as a radio galaxy whose jet is undergoing kink instability. This scenario is supported by recent MHD simulations of unstable jets that show remarkable similar features (e.g. the ribs)
7/8
7/8
We searched for dependencies of the radio activity of cluster members with the distance from the cluster center and velocity offset from the BCG. Although our results did not reveal any strong trends, this type of analysis could prove insightful in other clusters...
6/8
6/8
April 24, 2025 at 6:25 AM
We searched for dependencies of the radio activity of cluster members with the distance from the cluster center and velocity offset from the BCG. Although our results did not reveal any strong trends, this type of analysis could prove insightful in other clusters...
6/8
6/8
Optical catalogs are used to identify cluster members and spiral galaxies, this allowed us to detect at least 6 jellyfish galaxies in Ophiuchus thanks to their extended radio continuum tails. These are the first detected in this nearby cluster lying at low Galactic latitude
5/8
5/8
April 24, 2025 at 6:25 AM
Optical catalogs are used to identify cluster members and spiral galaxies, this allowed us to detect at least 6 jellyfish galaxies in Ophiuchus thanks to their extended radio continuum tails. These are the first detected in this nearby cluster lying at low Galactic latitude
5/8
5/8
In addition to the diffuse sources, the cluster hosts numerous tailed radio galaxies. Some are due to AGN (WATs and NATs) and others to SFGs that are undergoing ram-pressure stripping (jellyfish). This collection shows all the types of tails that one can find in Ophiuchus
4/8
4/8
April 24, 2025 at 6:25 AM
In addition to the diffuse sources, the cluster hosts numerous tailed radio galaxies. Some are due to AGN (WATs and NATs) and others to SFGs that are undergoing ram-pressure stripping (jellyfish). This collection shows all the types of tails that one can find in Ophiuchus
4/8
4/8
In addition to the mini halo, the cluster hosts a roundish extended emission that is believed to trace a fossil AGN lobe that has inflated a giant cavity in the ICM. The diffuse emission is recovered at higher significance in the low resolution images.
3/8
3/8
April 24, 2025 at 6:25 AM
In addition to the mini halo, the cluster hosts a roundish extended emission that is believed to trace a fossil AGN lobe that has inflated a giant cavity in the ICM. The diffuse emission is recovered at higher significance in the low resolution images.
3/8
3/8
We report the detection of thin emission threads embedded within the mini halo. These features are part of an emerging population of narrow radio filaments observed in the ICM, whose origin remains unclear (e.g. do they trace magnetic field lines stretched by sloshing?)
2/8
2/8
April 24, 2025 at 6:25 AM
We report the detection of thin emission threads embedded within the mini halo. These features are part of an emerging population of narrow radio filaments observed in the ICM, whose origin remains unclear (e.g. do they trace magnetic field lines stretched by sloshing?)
2/8
2/8
Paper accepted, today on arXiv (w/ @fabiogasta+)! We studied the Ophiuchus cluster, a massive sloshing system in the local Universe, with @SKA_Africa MeerKAT L band. The main discoveries are the detection of synchrotron threads and jellyfish galaxies
1/8
arxiv.org/abs/2504.16158
1/8
arxiv.org/abs/2504.16158
April 24, 2025 at 6:25 AM
Paper accepted, today on arXiv (w/ @fabiogasta+)! We studied the Ophiuchus cluster, a massive sloshing system in the local Universe, with @SKA_Africa MeerKAT L band. The main discoveries are the detection of synchrotron threads and jellyfish galaxies
1/8
arxiv.org/abs/2504.16158
1/8
arxiv.org/abs/2504.16158
Lensing study of the Bullet cluster, by Cha+
JWST imaging is used to reconstruct the mass distribution in the system which appears more complex than previously thought. A possible bridge of ICL is detected between the two main colliding systems.
arxiv.org/abs/2503.21870
JWST imaging is used to reconstruct the mass distribution in the system which appears more complex than previously thought. A possible bridge of ICL is detected between the two main colliding systems.
arxiv.org/abs/2503.21870
March 31, 2025 at 6:46 AM
Lensing study of the Bullet cluster, by Cha+
JWST imaging is used to reconstruct the mass distribution in the system which appears more complex than previously thought. A possible bridge of ICL is detected between the two main colliding systems.
arxiv.org/abs/2503.21870
JWST imaging is used to reconstruct the mass distribution in the system which appears more complex than previously thought. A possible bridge of ICL is detected between the two main colliding systems.
arxiv.org/abs/2503.21870