Andrea Botteon (@and_botteon) 's Twitter Profile
Andrea Botteon

@and_botteon

Astrophysicist at @IRA_INAF. Mainly dealing with colliding galaxy clusters, merger shocks and their radio outcome (@LOFAR). Also at andreabotteon.bsky.social

ID: 948995274961309697

calendar_today04-01-2018 19:11:19

2,2K Tweet

920 Followers

487 Following

Dr. James Beattie (@astro_magnetism) 's Twitter Profile Photo

The cascade of kinetic and magnetic energy from large to small scales in galactic-style turbulence behaves significantly different to the theoretical models that we usually assume work. nature.com/articles/s4155… Published in Nature Astronomy.

Overleaf (@overleaf) 's Twitter Profile Photo

āš ļø Attention: The site is currently down. Our engineering team is investigating. We will update as soon as possible. You can track progress here: status.overleaf.com Sorry for any inconvenience.

Dr Tessa Vernstrom (@tvern23) 's Twitter Profile Photo

If there’s any #astrotwitter folks left here check out two new papers on arxiv today description the #ASKAP #EMU survey arxiv.org/abs/2505.08271 and the #POSSUM survey arxiv.org/abs/2505.08272

Andrea Botteon (@and_botteon) 's Twitter Profile Photo

Thin filaments in the tails of A2255, by Emanuele De Rubeis+ (w/ myself++) A2255 is known to be a "mess" (arxiv.org/abs/2006.04808). The new Low Frequency Array-VLBI images add further complexity in the system, this time revealing small-scale structures in its radio galaxies arxiv.org/abs/2505.13595

Thin filaments in the tails of A2255, by <a href="/e_derubeis/">Emanuele De Rubeis</a>+ (w/ myself++)
A2255 is known to be a "mess" (arxiv.org/abs/2006.04808). The new <a href="/LOFAR/">Low Frequency Array</a>-VLBI images add further complexity in the system, this time revealing small-scale structures in its radio galaxies
arxiv.org/abs/2505.13595
Andrea Botteon (@and_botteon) 's Twitter Profile Photo

The central region of A3667 in hard X-rays, by Mohammad Mirakhor+Stephen A Walker A NASA NuSTAR mission 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

The central region of A3667 in hard X-rays, by <a href="/MSMirakhor/">Mohammad Mirakhor</a>+<a href="/astroswalker/">Stephen A Walker</a>
A <a href="/NASANuSTAR/">NASA NuSTAR mission</a> observation of the cluster is presented. The spectrum is better described by a 2T thermal model. An updated limit of B &gt; 0.2 muG is provided from the lack of IC emission
arxiv.org/abs/2505.20453
MEDIA INAF (@mediainaf) 's Twitter Profile Photo

Vanno ad Andrea Botteon e a Massimiliano Parente i due premi da duemila euro ciascuno della SAIt consegnati oggi a Firenze. Congratulazioni! media.inaf.it/2025/06/06/pre…

Kostas Migkas (@kmigkas) 's Twitter Profile Photo

šŸ“¢Paper and press releases day! We report the first-ever unambiguous detection of WHIM/missing baryons in a single cosmic filament using ESA XMM-Newton and JAXA(Japan Aerospace Exploration Agency) Suzaku data! It's the first time observations agree with LCDM simulations for the nature of WHIM aanda.org/component/cont…

Andrea Botteon (@and_botteon) 's Twitter Profile Photo

MeerKAT observations of CHEX-MATE clusters, by Balboni+ (w/ Fabio Gastaldello, Rossella Cassano, Giacomo Riva, Max Gaspari, Mariachiara Rossetti, 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

MeerKAT observations of CHEX-MATE clusters, by Balboni+ (w/ <a href="/fabiogasta/">Fabio Gastaldello</a>, <a href="/roxycas/">Rossella Cassano</a>, <a href="/GiacomoRiva7/">Giacomo Riva</a>, <a href="/max_gasp/">Max Gaspari</a>, <a href="/mcrossetti_twit/">Mariachiara Rossetti</a>, 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
Andrea Botteon (@and_botteon) 's Twitter Profile Photo

The magnetic field in A2142, by Pagliotta+ (w/ Chiara Stuardi, FraLoi++) 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

The magnetic field in A2142, by Pagliotta+ (w/ <a href="/CStuardi/">Chiara Stuardi</a>, <a href="/FraLoi1/">FraLoi</a>++)
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
Andrea Botteon (@and_botteon) 's Twitter Profile Photo

.XRISM 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 href="/XRISM_jp/">XRISM</a> obs of the Ophiuchus cluster, by Fujita+
A low velocity dispersion is measured in the inner and outer regions (115 km/s at &lt;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