From elia.battistelli at roma1.infn.it  Fri Dec  1 10:23:16 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Fri, 01 Dec 2017 10:23:16 +0100
Subject: [astroseminar@Sapienza] today at 13:00: Andreas Krut
Message-ID: <6d4c7510e6a0e8ea1d5376a5ff788ce8@roma1.infn.it>

Title: Novel constraints on fermionic dark matter from the Galactic 
observables
Speaker:  Andreas Krut
Institution: ICRANet
Date: Friday, 1 December 2017
Time: 1:00pm
Location: Aula 8, Fermi Building, Dept. of Physics, Sapienza University

Abstract:
It has been recently introduced a new model for the distribution of 
dark matter (DM) in galaxies, the Ruffini-Arguelles-Rueda (RAR) model, 
based on a self-gravitating system of massive fermions at finite 
temperatures. The RAR model, for fermion masses above keV, successfully 
describes the DM halos in galaxies, and predicts the existence of a 
denser quantum core towards the center of each configuration.  We 
demonstrate here that, for a fermion mass in the range 48 keV/c2?m?345 
keV/c2 , the DM distribution obtained from the RAR model fulfills the 
most recent data of the Milky Way rotation curves, and predicts the 
existence of a dense quantum core of 4?106M?within the S2-star 
pericenter. In addition, the dense quantum core represents an 
alternative to the central black hole (BH) scenario for SgrA*.

Questo seminario fa parte di una serie di incontri tipo "Brown Bag 
Lunch Meeting on Relativistic Astrophysics?. Seguono maggiori dettagli a 
tal proposito.

The "brown bag lunch" was instituted, in frugal time, at princeton in 
the Joseph Henry laboratory. They were encounters occurring in John 
Archibald Wheeler office:  lasting less than one hour and covering, 
every week, the latest results and possibly illustrated by new visitors. 
Both the theory group around Wheeler and the experimental group around 
Bob Dicke where participating. Later, as the topics became more 
favourable, they were extended to the astrophysics department (Karl 
Schwarzschild and Jerry Ostriker) and to the IAS (Freeman Dyson). The 
creation  of a sumptuous cafeteria at the IAS did create a more 
comfortable setting: these weekly meetings did not surpass the positive 
effects of the initial more frugal meetings. The transfer to Caltech of 
Princeton faculties including Kip Thorne permitted the prosecution of 
this tradition in California, equaly successfully. Since our groups have 
become larger in la Sapienza we (Paolo de Bernardis, cosmology, Fulvio 
Ricci, gravitational waves, and Remo Ruffini, gravitationally collapsed 
objects) have decided to start the "brown bag lunch" in relativistic 
astrophysics and cosmology in the physics department. The first meeting 
will be held on Friday 24 November in aula Rasetti at 1 pm and the topic 
will be the on equations of state of binary neutron-star merger.
Everyone interested is welcome to partecipate. Please bring your lunch. 
american coffee will be offered.




From elia.battistelli at roma1.infn.it  Fri Dec  1 16:47:06 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Fri, 01 Dec 2017 16:47:06 +0100
Subject: [astroseminar@Sapienza] 11/12/2017 at 16:00: Alessandro Schillaci
Message-ID: <a0fac99f7321d1c0bf67fca841018b27@roma1.infn.it>

Title: BICEP-Array: the next stage of CMB degree angular scale 
observations
Speaker:  Alessandro Schillaci
Institution: California Institute of Technology
Date: Monday, 11 December 2017
Time: 4:00pm
Location: Aula Conversi, Marconi Building, Dept. of Physics, Sapienza 
University

Abstract:
	BICEP Array, the Stage-3 instrument of the BICEP/Keck program, 
comprises four multi-frequency telescopes that will be deployed at the 
South Pole Station between 2018-2021. The 4 receivers  will observe 
simultaneously the degree-scale polarization of the Cosmic  Microwave 
Background and its Galactic foregrounds, ultimately improving the 
sensitivity to the primordial B-mode signal by one order of magnitude 
over the current most stringent limits (BK14).
	The 1st receiver, which is currently being built, will operate at 30 
and 40GHz to constrain the synchrotron foreground in the BK sky patch.  
It will be followed by the 95GHz  and the 150GHz receivers and completed 
by the 220/270GHz receiver, bringing the total count of 
background-limited detectors to about  40,000. In this talk, I will 
present an overview of the instrument,  focusing on the ongoing 30/40GHz 
receiver development, and particularly on the improvements on its 
thermal filtering, magnetic shielding, focal plane and detector design. 
I will also show the predicted constraints on the synchrotron foreground 
that this first low-frequency receiver will bring after 1+ years of 
science operations.

web: https://agenda.infn.it/conferenceDisplay.py?confId=14553


From elia.battistelli at roma1.infn.it  Fri Dec  1 16:50:20 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Fri, 01 Dec 2017 16:50:20 +0100
Subject: [astroseminar@Sapienza] 06/12/2017 at 16:00: Rudenko Valentin N.
Message-ID: <32a53ec59e854d9bb7fb4248e5c79479@roma1.infn.it>

Title: Gravitational Red Shift effect measurement with orbital probe
Speaker:  Rudenko Valentin N.
Institution: SAI MSU, Moscow
Date: Wednesday, 6 December 2017
Time: 4:00pm
Location: Aula Rasetti, Marconi Building, Dept. of Physics, Sapienza 
University

Abstract:
At present the Radioastron (RA) Earth's satellite having very elliptic 
orbit is used for probing of the gravitational red shift effect [1,2]. 
Objective of this test consists in the enhancing accuracy of measurement 
to prove the correspondence of the effect to the Einstein's theory at 
one order of value better then in was done in the GP-A experiment [3 ]. 
There are two H-masers in disposal, one at the board RA and other at the 
Land Tracking Station (LTS). One can compare its mutual time rate using 
communication radio links between RA and LTS. In contrast with the GP-A 
experiment for RA there is a possibility of measurement repetition and 
accumulation of data in the process of orbital circulation. It could be 
resulted in increasing of the integral accuracy. Receipt for a 
compensation of the coherent hindrances (Doppler, troposphere and 
ionosphere influence) developed during GP-A mission consists in 
simultaneously using the two modes communication of the LTS with RA: one 
way (H-maser) and two ways (Coherent) modes. However such opportunity 
was not foreseen for RA. Only a periodic switching between these modes 
is available.
    In this talk we investigate the achievable accuracy using a special 
algorithm of red shift extraction associated with technical specific of 
the RA satellite. Some experimental illustrations having been got during 
of RA functioning are presented as well as preliminary results of the 
red shift effect measurement.

References
1.	 A.V. Biriukov, V.L. Kauts, V.V. Kulagin, D.A. Litvinov, V.N. 
Rudenko,
Gravitational redshift test with the space radio telescope 
"RadioAstron", Astron. Rep. 58(11) (2014) 783-795,
http://dx.doi.org/10.1134/S1063772914110018
2.	2. D. A. Litvinov, V. N. Rudenko, A. V. Alakoz  et al Probing the
gravitational redshift with an Earth-orbiting satellite. Physics 
Letters A  v
381  (2017)
3.	3. R.F.C. Vessot, M.W. Levine, E.M. Mattison, et al.  Test of 
relativistic
gravitation with a space-borne hydrogen maser, Phys. Rev. Lett. 45 
(1980) 2081-2084, http://dx.doi.org/10.1103/PhysRevLett.45.2081

web: https://agenda.infn.it/conferenceDisplay.py?confId=14531


From elia.battistelli at roma1.infn.it  Wed Dec  6 12:57:42 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Wed, 06 Dec 2017 12:57:42 +0100
Subject: [astroseminar@Sapienza] today at 16:00: Rudenko Valentin N.
Message-ID: <75e9e63a1017895b24dad38f62cbb610@roma1.infn.it>

Title: Gravitational Red Shift effect measurement with orbital probe
Speaker:  Rudenko Valentin N.
Institution: SAI MSU, Moscow
Date: Wednesday, 6 December 2017
Time: 4:00pm
Location: Aula Rasetti, Marconi Building, Dept. of Physics, Sapienza 
University

Abstract:
At present the Radioastron (RA) Earth's satellite having very elliptic 
orbit is used for probing of the gravitational red shift effect [1,2]. 
Objective of this test consists in the enhancing accuracy of measurement 
to prove the correspondence of the effect to the Einstein's theory at 
one order of value better then in was done in the GP-A experiment [3 ]. 
There are two H-masers in disposal, one at the board RA and other at the 
Land Tracking Station (LTS). One can compare its mutual time rate using 
communication radio links between RA and LTS. In contrast with the GP-A 
experiment for RA there is a possibility of measurement repetition and 
accumulation of data in the process of orbital circulation. It could be 
resulted in increasing of the integral accuracy. Receipt for a 
compensation of the coherent hindrances (Doppler, troposphere and 
ionosphere influence) developed during GP-A mission consists in 
simultaneously using the two modes communication of the LTS with RA: one 
way (H-maser) and two ways (Coherent) modes. However such opportunity 
was not foreseen for RA. Only a periodic switching between these modes 
is available.
    In this talk we investigate the achievable accuracy using a special 
algorithm of red shift extraction associated with technical specific of 
the RA satellite. Some experimental illustrations having been got during 
of RA functioning are presented as well as preliminary results of the 
red shift effect measurement.

References
1.	 A.V. Biriukov, V.L. Kauts, V.V. Kulagin, D.A. Litvinov, V.N. 
Rudenko,
Gravitational redshift test with the space radio telescope 
"RadioAstron", Astron. Rep. 58(11) (2014) 783-795,
http://dx.doi.org/10.1134/S1063772914110018
2.	2. D. A. Litvinov, V. N. Rudenko, A. V. Alakoz  et al Probing the
gravitational redshift with an Earth-orbiting satellite. Physics 
Letters A  v
381  (2017)
3.	3. R.F.C. Vessot, M.W. Levine, E.M. Mattison, et al.  Test of 
relativistic
gravitation with a space-borne hydrogen maser, Phys. Rev. Lett. 45 
(1980) 2081-2084, http://dx.doi.org/10.1103/PhysRevLett.45.2081

web: https://agenda.infn.it/conferenceDisplay.py?confId=14531


From elia.battistelli at roma1.infn.it  Thu Dec  7 10:57:24 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Thu, 07 Dec 2017 10:57:24 +0100
Subject: [astroseminar@Sapienza] 11/12/2017 at 16:00: Alessandro Schillaci
 (REMOTE CONNECTION AVAILABLE)
Message-ID: <68ce852f7077741c4bb46002cda59e34@roma1.infn.it>


NOTE: due to the multiple requests an hangouts connection will be 
available for this talk.

Title: BICEP-Array: the next stage of CMB degree angular scale 
observations
Speaker:  Alessandro Schillaci
Institution: California Institute of Technology
Date: Monday, 11 December 2017
Time: 4:00pm
Location: Aula Conversi, Marconi Building, Dept. of Physics, Sapienza 
University
REMOTE CONNECTION: hangouts link 
https://hangouts.google.com/call/4RSq3kUQWxkbbR0s6WL0AAEI (note that 
hangouts has issues with Firefox plug in...better use other browser like 
Safari, Chrome, Explorer...).
Direct connection for any @uniroma1.it accounts; connection available 
on request for any other @gmail accounts...please send requests to 
elia.battistelli at uniroma1.it .

Abstract:
BICEP Array, the Stage-3 instrument of the BICEP/Keck program, 
comprises four multi-frequency telescopes that will be deployed at the 
South Pole Station between 2018-2021. The 4 receivers  will observe 
simultaneously the degree-scale polarization of the Cosmic  Microwave 
Background and its Galactic foregrounds, ultimately improving the 
sensitivity to the primordial B-mode signal by one order of magnitude 
over the current most stringent limits (BK14).
The 1st receiver, which is currently being built, will operate at 30 
and 40GHz to constrain the synchrotron foreground in the BK sky patch.  
It will be followed by the 95GHz  and the 150GHz receivers and completed 
by the 220/270GHz receiver, bringing the total count of 
background-limited detectors to about  40,000. In this talk, I will 
present an overview of the instrument,  focusing on the ongoing 30/40GHz 
receiver development, and particularly on the improvements on its 
thermal filtering, magnetic shielding, focal plane and detector design. 
I will also show the predicted constraints on the synchrotron foreground 
that this first low-frequency receiver will bring after 1+ years of 
science operations.

web: https://agenda.infn.it/conferenceDisplay.py?confId=14553


From elia.battistelli at roma1.infn.it  Mon Dec 11 10:17:47 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Mon, 11 Dec 2017 10:17:47 +0100
Subject: [astroseminar@Sapienza] today at 16:00: Alessandro Schillaci
	(REMOTE CONNECTION AVAILABLE)
Message-ID: <c25ddf822c456f89a3413cdab9f8a6e0@roma1.infn.it>

NOTE: due to the multiple requests an hangouts connection will be 
available for this talk.

Title: BICEP-Array: the next stage of CMB degree angular scale 
observations
Speaker:  Alessandro Schillaci
Institution: California Institute of Technology
Date: Monday, 11 December 2017
Time: 4:00pm
Location: Aula Conversi, Marconi Building, Dept. of Physics, Sapienza 
University
REMOTE CONNECTION: hangouts link 
https://hangouts.google.com/call/4RSq3kUQWxkbbR0s6WL0AAEI (note that 
hangouts has issues with Firefox plug in...better use other browser like 
Safari, Chrome, Explorer...).
Direct connection for any @uniroma1.it accounts; connection available 
on request for any other @gmail accounts...please send requests to 
elia.battistelli at uniroma1.it .

Abstract:
BICEP Array, the Stage-3 instrument of the BICEP/Keck program, 
comprises four multi-frequency telescopes that will be deployed at the 
South Pole Station between 2018-2021. The 4 receivers  will observe 
simultaneously the degree-scale polarization of the Cosmic  Microwave 
Background and its Galactic foregrounds, ultimately improving the 
sensitivity to the primordial B-mode signal by one order of magnitude 
over the current most stringent limits (BK14).
The 1st receiver, which is currently being built, will operate at 30 
and 40GHz to constrain the synchrotron foreground in the BK sky patch.  
It will be followed by the 95GHz  and the 150GHz receivers and completed 
by the 220/270GHz receiver, bringing the total count of 
background-limited detectors to about  40,000. In this talk, I will 
present an overview of the instrument,  focusing on the ongoing 30/40GHz 
receiver development, and particularly on the improvements on its 
thermal filtering, magnetic shielding, focal plane and detector design. 
I will also show the predicted constraints on the synchrotron foreground 
that this first low-frequency receiver will bring after 1+ years of 
science operations.

web: https://agenda.infn.it/conferenceDisplay.py?confId=14553


From elia.battistelli at roma1.infn.it  Mon Dec 11 16:05:32 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Mon, 11 Dec 2017 16:05:32 +0100
Subject: [astroseminar@Sapienza] now: Alessandro Schillaci (REMOTE
 CONNECTION AVAILABLE-PRESENTATION LINK)
Message-ID: <782e72476828eb2f89bc42f08d895fe1@roma1.infn.it>


PRESENTATION HERE: 
https://www.dropbox.com/s/w3x8wx6c607pfn5/Talk_Roma.pdf?dl=0

NOTE: due to the multiple requests an hangouts connection will be 
available for this talk.

Title: BICEP-Array: the next stage of CMB degree angular scale 
observations
Speaker:  Alessandro Schillaci
Institution: California Institute of Technology
Date: Monday, 11 December 2017
Time: 4:00pm
Location: Aula Conversi, Marconi Building, Dept. of Physics, Sapienza 
University
REMOTE CONNECTION: hangouts link 
https://hangouts.google.com/call/4RSq3kUQWxkbbR0s6WL0AAEI (note that 
hangouts has issues with Firefox plug in...better use other browser like 
Safari, Chrome, Explorer...).
Direct connection for any @uniroma1.it accounts; connection available 
on request for any other @gmail accounts...please send requests to 
elia.battistelli at uniroma1.it .

Abstract:
BICEP Array, the Stage-3 instrument of the BICEP/Keck program, 
comprises four multi-frequency telescopes that will be deployed at the 
South Pole Station between 2018-2021. The 4 receivers  will observe 
simultaneously the degree-scale polarization of the Cosmic  Microwave 
Background and its Galactic foregrounds, ultimately improving the 
sensitivity to the primordial B-mode signal by one order of magnitude 
over the current most stringent limits (BK14).
The 1st receiver, which is currently being built, will operate at 30 
and 40GHz to constrain the synchrotron foreground in the BK sky patch.  
It will be followed by the 95GHz  and the 150GHz receivers and completed 
by the 220/270GHz receiver, bringing the total count of 
background-limited detectors to about  40,000. In this talk, I will 
present an overview of the instrument,  focusing on the ongoing 30/40GHz 
receiver development, and particularly on the improvements on its 
thermal filtering, magnetic shielding, focal plane and detector design. 
I will also show the predicted constraints on the synchrotron foreground 
that this first low-frequency receiver will bring after 1+ years of 
science operations.

web: https://agenda.infn.it/conferenceDisplay.py?confId=14553


From elia.battistelli at roma1.infn.it  Fri Dec 15 14:21:56 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Fri, 15 Dec 2017 14:21:56 +0100
Subject: [astroseminar@Sapienza] 18/12/2017 at 14:00: New physics with
	gravitational waves
Message-ID: <7fd64fc41595589c74f3ded6f9ecbde6@roma1.infn.it>

Event on: New physics with gravitational waves
Date: Monday, 18 December 2017
Time: 2:00pm-6:00pm
Location: Aula 7, Fermi Building, Dept. of Physics, Sapienza University

Agenda:
14:00 - 14:05 Introduction 5'
Speaker: 	Fulvio Ricci (ROMA1)
14:05 - 14:40 Summary of the results with the O1 and O2 scientific runs 
of advanced LIGO and Virgo and future plans. 35'
Speaker: 	Piero Rapagnani (ROMA1)
14:40 - 15:15 The elettromagnetic follow-up of GW170817. What we 
learned and what can we expect in the future. 35'
Speaker: 	S. Piranomonte (INAF)
15:15 - 15:50 Integral results from GW170817 and future perspectives. 
35'
Speaker: 	Prof. Pietro Ubertini (IAPS-INAF)
15:50 - 16:25 Gravitational waves as a probe of fundamental physics. 
35'
Speaker: 	Valeria Ferrari (ROMA1)
16:25 - 17:00 Coffee break
17:00 - 18:00 Round table: ?Gravitational waves: where do we go from 
here?

web: https://agenda.infn.it/conferenceDisplay.py?confId=14674

From elia.battistelli at roma1.infn.it  Mon Dec 18 12:44:40 2017
From: elia.battistelli at roma1.infn.it (Elia Battistelli)
Date: Mon, 18 Dec 2017 12:44:40 +0100
Subject: [astroseminar@Sapienza] today at 14:00: New physics with
	gravitational waves
Message-ID: <d6dd751f1013db418e1406e098a23e9f@roma1.infn.it>

Event on: New physics with gravitational waves
Date: Monday, 18 December 2017
Time: 2:00pm-6:00pm
Location: Aula 7, Fermi Building, Dept. of Physics, Sapienza University

Agenda:
14:00 - 14:05 Introduction 5'
Speaker: 	Fulvio Ricci (ROMA1)
14:05 - 14:40 Summary of the results with the O1 and O2 scientific runs 
of advanced LIGO and Virgo and future plans. 35'
Speaker: 	Piero Rapagnani (ROMA1)
14:40 - 15:15 The elettromagnetic follow-up of GW170817. What we 
learned and what can we expect in the future. 35'
Speaker: 	S. Piranomonte (INAF)
15:15 - 15:50 Integral results from GW170817 and future perspectives. 
35'
Speaker: 	Prof. Pietro Ubertini (IAPS-INAF)
15:50 - 16:25 Gravitational waves as a probe of fundamental physics. 
35'
Speaker: 	Valeria Ferrari (ROMA1)
16:25 - 17:00 Coffee break
17:00 - 18:00 Round table: ?Gravitational waves: where do we go from 
here?

web: https://agenda.infn.it/conferenceDisplay.py?confId=14674


