From ftadd at astro.su.se  Thu Feb  8 10:40:50 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 8 Feb 2018 10:40:50 +0100
Subject: [Okc-wp4] EO meeting on Feb 15th
Message-ID: <5FC20870-2661-44DF-B17C-18B781C92EFF@astro.su.se>


Hi all,

time to restart our EO meetings,
next one will be on Feb 15th, at 13:00, in the KTH meeting room on floor 5.
We will have a talk by Dennis Alp, here the title and the abstract:

%%%%%%%%%%%%%%%%%

Title: 
Multiwavelength Limits on a Compact Object in SN 1987A 30 Years After Explosion

Abstract: 
The compact object produced by SN 1987A has not yet been detected despite 30 years of searches spanning the entire electromagnetic spectrum. I will present new limits on a point source in the debris of SN 1987A obtained from recent observations. Limits are obtained using ALMA images at millimeter wavelengths; VLT NACO images and SINFONI spectra in NIR; HST WFC3 images and STIS spectra in optical and UV; and Chandra in X-rays. New constraints on the amount of absorption at X-ray energies are computed using 3D explosion models. Limits at other frequencies are taken from literature for complete coverage of the entire electromagnetic spectrum. We also investigate the total energy budget of the central ejecta and find that the allowed bolometric luminosity of the compact object is 240 Lsun. We discuss how these new limits constrain the physical properties of the compact object and prospects for detecting the compact object with future facilities.

%%%%%%%%%%%%%%%%%

cheers

/Francesco

From ftadd at astro.su.se  Thu Feb 15 08:50:10 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 15 Feb 2018 08:50:10 +0100
Subject: [Okc-wp4] Reminder: EO meeting on Feb 15th
In-Reply-To: <5FC20870-2661-44DF-B17C-18B781C92EFF@astro.su.se>
References: <5FC20870-2661-44DF-B17C-18B781C92EFF@astro.su.se>
Message-ID: <13405B8C-CD69-4359-B750-2DBD2F21A8C3@astro.su.se>

TODAY!!!

> On 8 Feb 2018, at 10:40, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> 
> Hi all,
> 
> time to restart our EO meetings,
> next one will be on Feb 15th, at 13:00, in the KTH meeting room on floor 5.
> We will have a talk by Dennis Alp, here the title and the abstract:
> 
> %%%%%%%%%%%%%%%%%
> 
> Title: 
> Multiwavelength Limits on a Compact Object in SN 1987A 30 Years After Explosion
> 
> Abstract: 
> The compact object produced by SN 1987A has not yet been detected despite 30 years of searches spanning the entire electromagnetic spectrum. I will present new limits on a point source in the debris of SN 1987A obtained from recent observations. Limits are obtained using ALMA images at millimeter wavelengths; VLT NACO images and SINFONI spectra in NIR; HST WFC3 images and STIS spectra in optical and UV; and Chandra in X-rays. New constraints on the amount of absorption at X-ray energies are computed using 3D explosion models. Limits at other frequencies are taken from literature for complete coverage of the entire electromagnetic spectrum. We also investigate the total energy budget of the central ejecta and find that the allowed bolometric luminosity of the compact object is 240 Lsun. We discuss how these new limits constrain the physical properties of the compact object and prospects for detecting the compact object with future facilities.
> 
> %%%%%%%%%%%%%%%%%
> 
> cheers
> 
> /Francesco


From ftadd at astro.su.se  Tue Feb 27 09:48:01 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Tue, 27 Feb 2018 09:48:01 +0100
Subject: [Okc-wp4] EO meeting on March 1st (PLEASE NOTE: new room A3:1003 !!)
Message-ID: <F1B1DB9E-8999-4D5C-8815-BDAE05964059@astro.su.se>

Hi all,

this Thursday, March 1st, we will have the second EO meeting of this year.

Leonardo Tartaglia will talk about “Exploding massive stars and impostors”.

Please note that this time the meeting will take place two floors down from the usual place,
in room A3:1003.

See you there!

/Francesco
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From ftadd at astro.su.se  Tue Feb 27 11:47:00 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Tue, 27 Feb 2018 11:47:00 +0100
Subject: [Okc-wp4] EO meeting on March 1st (PLEASE NOTE: new room
 A3:1003 !!)
In-Reply-To: <F1B1DB9E-8999-4D5C-8815-BDAE05964059@astro.su.se>
References: <F1B1DB9E-8999-4D5C-8815-BDAE05964059@astro.su.se>
Message-ID: <73AF5540-99AB-46F9-B859-D0F98B47DBFD@astro.su.se>

I forgot to mention that the time of the meeting is the usual one, at 13:00,

cheers

/Francesco

> On 27 Feb 2018, at 09:48, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> this Thursday, March 1st, we will have the second EO meeting of this year.
> 
> Leonardo Tartaglia will talk about “Exploding massive stars and impostors”.
> 
> Please note that this time the meeting will take place two floors down from the usual place,
> in room A3:1003.
> 
> See you there!
> 
> /Francesco
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Thu Mar  1 11:18:05 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 1 Mar 2018 11:18:05 +0100
Subject: [Okc-wp4] EO meeting on March 1st (PLEASE NOTE: new room
 A3:1003 !!)
In-Reply-To: <73AF5540-99AB-46F9-B859-D0F98B47DBFD@astro.su.se>
References: <F1B1DB9E-8999-4D5C-8815-BDAE05964059@astro.su.se>
 <73AF5540-99AB-46F9-B859-D0F98B47DBFD@astro.su.se>
Message-ID: <44FE40D8-B6D1-4AB3-AD11-468EDB09B64F@astro.su.se>

Today!!

remember the room is NOT the usual one, instead we meet on the third floor in A3:1003

cheers

/Francesco

> On 27 Feb 2018, at 11:47, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> I forgot to mention that the time of the meeting is the usual one, at 13:00,
> 
> cheers
> 
> /Francesco
> 
>> On 27 Feb 2018, at 09:48, Francesco Taddia <ftadd at astro.su.se <mailto:ftadd at astro.su.se>> wrote:
>> 
>> Hi all,
>> 
>> this Thursday, March 1st, we will have the second EO meeting of this year.
>> 
>> Leonardo Tartaglia will talk about “Exploding massive stars and impostors”.
>> 
>> Please note that this time the meeting will take place two floors down from the usual place,
>> in room A3:1003.
>> 
>> See you there!
>> 
>> /Francesco
>> 
>> -------------------------------------------------
>> okc-wp4 at albanova.se <mailto:okc-wp4 at albanova.se> mailing list
> 
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Tue Mar 13 14:56:30 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Tue, 13 Mar 2018 14:56:30 +0100
Subject: [Okc-wp4] EO meeting on Thursday (15th of March, 13:00)
Message-ID: <2920DFC9-A54F-4032-8A98-84B6FEE45089@astro.su.se>

Hi all, 

next meeting on thursday we will have Ragnhild Lunnan speaking about her recent work on a super-luminous supernova.
Please note that the meeting will be in the usual KTH room on the 5th floor with a view, 13:00-14:00.

Here title and abstract:

%%%%%%%%%

Title: A Circumstellar Shell around a Superluminous Supernova Revealed in a Light Echo

Abstract: Superluminous supernovae (SLSNe) are a rare class of transients with peak luminosities 10-100 times those of normal core-collapse and Type Ia SNe, and whose progenitors and energy sources are still debated. Here, I will report on a surprising result from our Keck late-time spectroscopic survey of SLSNe: the discovery of a shell of circumstellar material (CSM) around the supernova, revealed by both absorption and subsequent re-emission in Mg II from the shell, in an “echo” of the SN light. The blueshift of the absorption lines allow us to measure the velocity of the CSM shell, while the time delay between the blueshifted and redshifted emission lines directly constrains the size of the shell. While pre-supernova mass loss is not uncommon in massive stars, this kind of observation is nearly unique, with the closest observed analogue being the ionization of the ring around SN1987A by the supernova flash. I will discuss both the circumstances that allowed us to observe it in this particular instance, and the implications for superluminous supernova progenitors and mass loss mechanisms. In this case, the high shell velocity (~3000 km/s) and implied time of the eruption (~40 years prior to explosion) may point to a pulsational pair-instability origin.
%%%%%%%%%

cheers

/Francesco


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From ftadd at astro.su.se  Thu Mar 15 10:04:59 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 15 Mar 2018 10:04:59 +0100
Subject: [Okc-wp4] Reminder:  EO meeting on Thursday (15th of March, 13:00)
In-Reply-To: <2920DFC9-A54F-4032-8A98-84B6FEE45089@astro.su.se>
References: <2920DFC9-A54F-4032-8A98-84B6FEE45089@astro.su.se>
Message-ID: <D7FC2EF8-03B7-42AA-9682-FB5EE1B95AB9@astro.su.se>



TODAY!!!!!


> On 13 Mar 2018, at 14:56, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all, 
> 
> next meeting on thursday we will have Ragnhild Lunnan speaking about her recent work on a super-luminous supernova.
> Please note that the meeting will be in the usual KTH room on the 5th floor with a view, 13:00-14:00.
> 
> Here title and abstract:
> 
> %%%%%%%%%
> 
> Title: A Circumstellar Shell around a Superluminous Supernova Revealed in a Light Echo
> 
> Abstract: Superluminous supernovae (SLSNe) are a rare class of transients with peak luminosities 10-100 times those of normal core-collapse and Type Ia SNe, and whose progenitors and energy sources are still debated. Here, I will report on a surprising result from our Keck late-time spectroscopic survey of SLSNe: the discovery of a shell of circumstellar material (CSM) around the supernova, revealed by both absorption and subsequent re-emission in Mg II from the shell, in an “echo” of the SN light. The blueshift of the absorption lines allow us to measure the velocity of the CSM shell, while the time delay between the blueshifted and redshifted emission lines directly constrains the size of the shell. While pre-supernova mass loss is not uncommon in massive stars, this kind of observation is nearly unique, with the closest observed analogue being the ionization of the ring around SN1987A by the supernova flash. I will discuss both the circumstances that allowed us to observe it in this particular instance, and the implications for superluminous supernova progenitors and mass loss mechanisms. In this case, the high shell velocity (~3000 km/s) and implied time of the eruption (~40 years prior to explosion) may point to a pulsational pair-instability origin.
> %%%%%%%%%
> 
> cheers
> 
> /Francesco
> 
> 
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Wed Apr 11 18:05:43 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Wed, 11 Apr 2018 18:05:43 +0200
Subject: [Okc-wp4] Next EO meeting on Thursday 19th of April
Message-ID: <28A86E42-4D69-43A5-A739-C8CA2E96A7ED@astro.su.se>

Dear all, 

on Thursday 19th of April at 13:15 (slightly later to avoid conflict with another meeting) we will have our next EO meeting,
 in the usual KTH meeting room on the 5th floor.

The speaker is Irvin Martinez Rodriguez, who is visiting in Stockholm. Below, title and abstract of his talk.

cheers

/Francesco

%%%%%%%%%%%%%%%%%%

Title: 
Towards the binary compact object formation as an effective field theory

Abstract: 
To solve  the dynamics of a pair of heavy and compact objects through the exchange of gravitational degrees of freedom and emitting gravitational waves we can set the problem in an effective field theory framework, in the non relativistic general relativity formulation known as effective field theory for extended objects. The two-body problem exhibits a clear separation of scales: The size of the compact objects, the orbital separation and the gravitational wavelength, all controlled by the same expansion parameter. This approach is a way of organizing systemastic expansions in powers of ratios of scales. We describe how to "integrate out" physics at each of the scales to obtain a theory with well defined rules for calculating observables. A possible extension of this idea to formulate the compact object formation in this framework is discussed.

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From ftadd at astro.su.se  Mon Apr 16 11:54:28 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 16 Apr 2018 11:54:28 +0200
Subject: [Okc-wp4] Next EO meeting on Thursday 19th of April (in A4:1003
 at 13:15)
In-Reply-To: <28A86E42-4D69-43A5-A739-C8CA2E96A7ED@astro.su.se>
References: <28A86E42-4D69-43A5-A739-C8CA2E96A7ED@astro.su.se>
Message-ID: <E466A3AF-CF43-4DD1-A280-0DD078334E21@astro.su.se>

Hi all,

We have a change in the room for our next EO meeting on thursday:
we will be in A4:1003 (the room right below the normal meeting room, on the 4th floor).

cheers

/Francesco



> On 11 Apr 2018, at 18:05, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Dear all, 
> 
> on Thursday 19th of April at 13:15 (slightly later to avoid conflict with another meeting) we will have our next EO meeting,
>  in the usual KTH meeting room on the 5th floor.
> 
> The speaker is Irvin Martinez Rodriguez, who is visiting in Stockholm. Below, title and abstract of his talk.
> 
> cheers
> 
> /Francesco
> 
> %%%%%%%%%%%%%%%%%%
> 
> Title: 
> Towards the binary compact object formation as an effective field theory
> 
> Abstract: 
> To solve  the dynamics of a pair of heavy and compact objects through the exchange of gravitational degrees of freedom and emitting gravitational waves we can set the problem in an effective field theory framework, in the non relativistic general relativity formulation known as effective field theory for extended objects. The two-body problem exhibits a clear separation of scales: The size of the compact objects, the orbital separation and the gravitational wavelength, all controlled by the same expansion parameter. This approach is a way of organizing systemastic expansions in powers of ratios of scales. We describe how to "integrate out" physics at each of the scales to obtain a theory with well defined rules for calculating observables. A possible extension of this idea to formulate the compact object formation in this framework is discussed.
> 
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Thu Apr 19 10:14:49 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 19 Apr 2018 10:14:49 +0200
Subject: [Okc-wp4] Next EO meeting on Thursday 19th of April (in A4:1003
 at 13:15)
In-Reply-To: <E466A3AF-CF43-4DD1-A280-0DD078334E21@astro.su.se>
References: <28A86E42-4D69-43A5-A739-C8CA2E96A7ED@astro.su.se>
 <E466A3AF-CF43-4DD1-A280-0DD078334E21@astro.su.se>
Message-ID: <EA57C78F-CB98-4F63-B50A-9049DE432EA1@astro.su.se>

Dear all,

this is a reminder for our EO meeting,
TODAY at 13:15 in A4:1003,

cheers

/Francesco

> On 16 Apr 2018, at 11:54, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> We have a change in the room for our next EO meeting on thursday:
> we will be in A4:1003 (the room right below the normal meeting room, on the 4th floor).
> 
> cheers
> 
> /Francesco
> 
> 
> 
>> On 11 Apr 2018, at 18:05, Francesco Taddia <ftadd at astro.su.se <mailto:ftadd at astro.su.se>> wrote:
>> 
>> Dear all, 
>> 
>> on Thursday 19th of April at 13:15 (slightly later to avoid conflict with another meeting) we will have our next EO meeting,
>>  in the usual KTH meeting room on the 5th floor.
>> 
>> The speaker is Irvin Martinez Rodriguez, who is visiting in Stockholm. Below, title and abstract of his talk.
>> 
>> cheers
>> 
>> /Francesco
>> 
>> %%%%%%%%%%%%%%%%%%
>> 
>> Title: 
>> Towards the binary compact object formation as an effective field theory
>> 
>> Abstract: 
>> To solve  the dynamics of a pair of heavy and compact objects through the exchange of gravitational degrees of freedom and emitting gravitational waves we can set the problem in an effective field theory framework, in the non relativistic general relativity formulation known as effective field theory for extended objects. The two-body problem exhibits a clear separation of scales: The size of the compact objects, the orbital separation and the gravitational wavelength, all controlled by the same expansion parameter. This approach is a way of organizing systemastic expansions in powers of ratios of scales. We describe how to "integrate out" physics at each of the scales to obtain a theory with well defined rules for calculating observables. A possible extension of this idea to formulate the compact object formation in this framework is discussed.
>> 
>> 
>> -------------------------------------------------
>> okc-wp4 at albanova.se <mailto:okc-wp4 at albanova.se> mailing list
> 
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Mon Apr 23 09:42:49 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 23 Apr 2018 09:42:49 +0200
Subject: [Okc-wp4] EO meeting on Thursday 26th of April
Message-ID: <A9B3E796-24A8-4694-B964-CE6D85F5C6B8@astro.su.se>

Hi all,

during our next EO meeting on 26/04/2018, at 13:00 in the KTH meeting room on the 5th floor,
we will have a talk by Cristina Barbarino. Here title and abstract:

Title: Stripped envelope supernovae from PTF and iPTF

Abstract: Stripped envelope supernovae (SESNe) are the result of the collapse of a massive star whose outer layer of hydrogen has been partially or completely removed. Two main scenario have been proposed for the progenitor channel: a single massive star or a binary system. They represent a quite rare class of supernovae (~34% of core-collapse) and only in the recent time with the upcoming of several surveys it was possible to build up a sample of objects being statistically significant. In this scenario, the Palomar Transient Factory (PTF) and the intermediate PTF (iPTF) bring their contributions; infact, unlike all their predecessors, those were untargeted surveys. The surveys took place through the use, mainly, of the P48 and P60 telescopes at the Palomar Observatory but several other facilities were involved to implement the collected data set (e.g. P200, NOT, LCOGT, Keck, Gemini...) on the window of time 2009-2016. These surveys have been a forerunner for the upcoming Zwicky Transient Facility (ZTF) which already saw its first light and will be fully operative in early 2018. I will present the SNe Ib/c sample found from PTF and iPTF. The analysis is mainly focused on the photometric dataset, in order to estimate the explosion parameters and to investigate the progenitor system.​

cheers

/Francesco

From ftadd at astro.su.se  Thu Apr 26 10:14:48 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 26 Apr 2018 10:14:48 +0200
Subject: [Okc-wp4] EO meeting on Thursday 26th of April
In-Reply-To: <A9B3E796-24A8-4694-B964-CE6D85F5C6B8@astro.su.se>
References: <A9B3E796-24A8-4694-B964-CE6D85F5C6B8@astro.su.se>
Message-ID: <BC461126-4BD1-4367-8D30-4C29509286A6@astro.su.se>

TODAY!!

> On 23 Apr 2018, at 09:42, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> during our next EO meeting on 26/04/2018, at 13:00 in the KTH meeting room on the 5th floor,
> we will have a talk by Cristina Barbarino. Here title and abstract:
> 
> Title: Stripped envelope supernovae from PTF and iPTF
> 
> Abstract: Stripped envelope supernovae (SESNe) are the result of the collapse of a massive star whose outer layer of hydrogen has been partially or completely removed. Two main scenario have been proposed for the progenitor channel: a single massive star or a binary system. They represent a quite rare class of supernovae (~34% of core-collapse) and only in the recent time with the upcoming of several surveys it was possible to build up a sample of objects being statistically significant. In this scenario, the Palomar Transient Factory (PTF) and the intermediate PTF (iPTF) bring their contributions; infact, unlike all their predecessors, those were untargeted surveys. The surveys took place through the use, mainly, of the P48 and P60 telescopes at the Palomar Observatory but several other facilities were involved to implement the collected data set (e.g. P200, NOT, LCOGT, Keck, Gemini...) on the window of time 2009-2016. These surveys have been a forerunner for the upcoming Zwicky Transient Facility (ZTF) which already saw its first light and will be fully operative in early 2018. I will present the SNe Ib/c sample found from PTF and iPTF. The analysis is mainly focused on the photometric dataset, in order to estimate the explosion parameters and to investigate the progenitor system.​
> 
> cheers
> 
> /Francesco


From ftadd at astro.su.se  Mon May 14 09:38:39 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 14 May 2018 09:38:39 +0200
Subject: [Okc-wp4] EO meeting on Thursday 17th of May
Message-ID: <0DC4D058-E69C-4BF2-B977-95D419D1266D@astro.su.se>

Hi all,

during our next EO meeting (13:00-14:00, May 17th, 5th floor KTH meeting room),
we will have Mattia Bulla talking about polarisation in macronovae. Here title and abstract:


Title: The origin of polarization in macronovae and the case of AT 2017gfo

Abstract: The gravitational wave event GW 170817 was due to the coalescence of two neutron stars and produced a transient electromagnetic source, labelled AT 2017gfo, that was target of a massive observational campaign. Together with photometric and spectroscopic observations, polarimetric measurements were also obtained. These data showed that the polarization detected from AT 2017gfo was consistent with being induced by dust in our Galaxy, thus suggesting that the intrinsic emission was at most weakly polarized (P < 0.4-0.5%). Polarimetry can be a powerful diagnostics of the geometry and emission processes of unresolved sources. In my talk, I will discuss a detailed analysis of the expected polarization from a macronova by means of 3D Monte Carlo radiative transfer simulations assuming a range of possible configurations, wavelengths, epochs and viewing angles. The main result is that the maximum polarization degree is relatively small (P < 1 %) at early times (1-2 days after the merger) and no polarization is expected at later times. Low polarization levels are expected at any epoch in the blue part of the spectrum and in the near-infrared with the best chances for a positive detection in the R-band. A clear dependence on the viewing angle allows us to derive independent constrains for the case of AT 2017gfo, which are fully consistent with estimates based on gravitational wave analysis.

cheers

/Francesco
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From ftadd at astro.su.se  Thu May 17 10:08:49 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 17 May 2018 10:08:49 +0200
Subject: [Okc-wp4] Reminder:  EO meeting on Thursday 17th of May
In-Reply-To: <0DC4D058-E69C-4BF2-B977-95D419D1266D@astro.su.se>
References: <0DC4D058-E69C-4BF2-B977-95D419D1266D@astro.su.se>
Message-ID: <95656074-CEB8-41EF-B92F-38D779FF31E8@astro.su.se>

TODAY!!!


> On 14 May 2018, at 09:38, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> during our next EO meeting (13:00-14:00, May 17th, 5th floor KTH meeting room),
> we will have Mattia Bulla talking about polarisation in macronovae. Here title and abstract:
> 
> 
> Title: The origin of polarization in macronovae and the case of AT 2017gfo
> 
> Abstract: The gravitational wave event GW 170817 was due to the coalescence of two neutron stars and produced a transient electromagnetic source, labelled AT 2017gfo, that was target of a massive observational campaign. Together with photometric and spectroscopic observations, polarimetric measurements were also obtained. These data showed that the polarization detected from AT 2017gfo was consistent with being induced by dust in our Galaxy, thus suggesting that the intrinsic emission was at most weakly polarized (P < 0.4-0.5%). Polarimetry can be a powerful diagnostics of the geometry and emission processes of unresolved sources. In my talk, I will discuss a detailed analysis of the expected polarization from a macronova by means of 3D Monte Carlo radiative transfer simulations assuming a range of possible configurations, wavelengths, epochs and viewing angles. The main result is that the maximum polarization degree is relatively small (P < 1 %) at early times (1-2 days after the merger) and no polarization is expected at later times. Low polarization levels are expected at any epoch in the blue part of the spectrum and in the near-infrared with the best chances for a positive detection in the R-band. A clear dependence on the viewing angle allows us to derive independent constrains for the case of AT 2017gfo, which are fully consistent with estimates based on gravitational wave analysis.
> 
> cheers
> 
> /Francesco
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Mon May 21 13:28:26 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 21 May 2018 13:28:26 +0200
Subject: [Okc-wp4] EO meeting this week on Thursday 24th
Message-ID: <2E5C9AA6-5620-4AC1-9574-2B7537A44303@astro.su.se>

Hi all,

two talks at the next EO meeting on Thursday 24th, 13:00, in the KTH meeting room (5th floor).
Here speakers, titles and abstracts:

1) Speaker: Magnus Axelsson

Title: Breaking the spectral degeneracies in black hole binaries with fast timing data

Abstract: The spectra of black hole binaries in the low/hard state are complex, with evidence for multiple different
 Comptonisation regions contributing to the hard X-rays, in addition to a cool disc component. However, it is difficult to
 constrain these components uniquely using spectral data alone. Using observations of Cygnus X-1, I will show that
 additional information from fast variability can break this degeneracy, and gives new insight into
 the physical processes active in the inner accretion flow.

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

2) Speaker: Giovanni Camelio

Title: Disk formation from the collapse of a rotating neutron star

Abstract:
An unstable rotating neutron star can collapse to a black hole.
A particle in the Innermost Stable Circular Orbit (ISCO) of this black hole has
the lowest possible angular momentum that prevents it to fall into the black hole.
If the matter of the unstable neutron star has everywhere a specific angular
momentum smaller than that of the ISCO, no particle will escape the collapse.
Using this criterion, we estimate the mass of the disk that might form in a
neutron star collapse for a variety of Equation Of States (EOSs).
We find that for all considered EOSs the disk mass is too low to generate gamma
ray bursts with significant energy.
We checked our estimates with general relativistic dynamical simulations.


%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

cheers

/Francesco




 

From ftadd at astro.su.se  Thu May 24 09:20:23 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 24 May 2018 09:20:23 +0200
Subject: [Okc-wp4] Reminder:  EO meeting this week on Thursday 24th
In-Reply-To: <2E5C9AA6-5620-4AC1-9574-2B7537A44303@astro.su.se>
References: <2E5C9AA6-5620-4AC1-9574-2B7537A44303@astro.su.se>
Message-ID: <7460471A-5C9E-4BE0-8879-FD4C87EE045B@astro.su.se>

TODAY!!!

> On 21 May 2018, at 13:28, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> two talks at the next EO meeting on Thursday 24th, 13:00, in the KTH meeting room (5th floor).
> Here speakers, titles and abstracts:
> 
> 1) Speaker: Magnus Axelsson
> 
> Title: Breaking the spectral degeneracies in black hole binaries with fast timing data
> 
> Abstract: The spectra of black hole binaries in the low/hard state are complex, with evidence for multiple different
> Comptonisation regions contributing to the hard X-rays, in addition to a cool disc component. However, it is difficult to
> constrain these components uniquely using spectral data alone. Using observations of Cygnus X-1, I will show that
> additional information from fast variability can break this degeneracy, and gives new insight into
> the physical processes active in the inner accretion flow.
> 
> %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
> 
> 2) Speaker: Giovanni Camelio
> 
> Title: Disk formation from the collapse of a rotating neutron star
> 
> Abstract:
> An unstable rotating neutron star can collapse to a black hole.
> A particle in the Innermost Stable Circular Orbit (ISCO) of this black hole has
> the lowest possible angular momentum that prevents it to fall into the black hole.
> If the matter of the unstable neutron star has everywhere a specific angular
> momentum smaller than that of the ISCO, no particle will escape the collapse.
> Using this criterion, we estimate the mass of the disk that might form in a
> neutron star collapse for a variety of Equation Of States (EOSs).
> We find that for all considered EOSs the disk mass is too low to generate gamma
> ray bursts with significant energy.
> We checked our estimates with general relativistic dynamical simulations.
> 
> 
> %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
> 
> cheers
> 
> /Francesco
> 
> 
> 
> 
> 
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list


From serena at fysik.su.se  Tue May 29 14:17:31 2018
From: serena at fysik.su.se (Serena Nobili)
Date: Tue, 29 May 2018 12:17:31 +0000
Subject: [Okc-wp4] Fwd: X-ray polarimetry seminar (Wednesday,
 1300) and thesis defence (Thursday, 1400).
References: <FD964859-4A4A-4F51-BADB-81327E01C182@kth.se>
Message-ID: <83A4163F-BA98-46FB-B7D4-07B2F83806BF@fysik.su.se>



From: Mark Pearce <pearce at kth.se<mailto:pearce at kth.se>>
Subject: X-ray polarimetry seminar (Wednesday, 1300) and thesis defence (Thursday, 1400).
Date: 28 May 2018 at 15:23:10 CEST
To: "Okc-wp4 at fysik.su.se<mailto:Okc-wp4 at fysik.su.se>" <Okc-wp4 at fysik.su.se<mailto:Okc-wp4 at fysik.su.se>>, "epi at particle.kth.se<mailto:epi at particle.kth.se>" <epi at particle.kth.se<mailto:epi at particle.kth.se>>, "exjobbare at particle.kth.se<mailto:exjobbare at particle.kth.se>" <exjobbare at particle.kth.se<mailto:exjobbare at particle.kth.se>>


Hej,

Herman Marshall (MIT) will give a seminar on X-ray polarimetry on Wednesday 30th May, 1300, in the KTH meeting room on the 5th floor. The abstract is appended below.

On Thursday, Herman will be the opponent for Victor Mikhalev’s Ph.D. Thesis defence (starting at 1400, FB42) - “Measurements of hard X-ray polarisation from the Crab and Cygnus X-1” (http://kth.diva-portal.org/smash/record.jsf?pid=diva2%3A1208715<http://kth.diva-portal.org/smash/record.jsf?pid=diva2:1208715>).

You are very welcome to both events!

        -Mark

---------------------------------------
Expanding the Field of X-ray Polarimetry

Herman Marshall, MIT

I will present several projects to measure the X-ray polarizations of astronomical sources over the next 5-10 years.  Previous observations were obtained in the 1970s for bright Galactic sources such as X-ray binaries and the Crab Nebula using a Bragg reflection from graphite crystals, limiting the measurements to 2.6 and 5.2 keV.  Recently, detections have been reported using Compton scattering at hard X-rays. An approved NASA mission is the Imaging X-ray Polarization Explorer (IXPE).  It would operate in the 2-8 keV range and is expected to launch in early 2021. It has an imaging capability, with a resolution of about a half arc-minute, and should detect X-ray polarizations as low as 1-5 percent for a dozen or more active galaxies, supernova remnants, neutron stars, and X-ray binaries during a mission lifetime of a few years. I will describe the instrument and some of the science goals.  I will also describe a design for a sounding rocket based polarimeter to work in the 0.2-0.6 keV band.  The method uses gratings developed at MIT and multilayer coated mirrors.  Potential targets include active galaxies, isolated neutron stars, and nearby black hole binaries in outburst.  The configuration is extensible to orbital use, possibly to be combined with other instruments to provide a bandpass from 0.2 to 50 keV.


------------------------------------
Mark Pearce
professor, Head of Physics Department

KTH Royal Institute of Technology
https://www.kth.se/profile/pearce











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From ftadd at astro.su.se  Fri Jun  1 15:31:23 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Fri, 1 Jun 2018 15:31:23 +0200
Subject: [Okc-wp4] Licentiate seminar, Monday June 4 at 10-12, FB42
Message-ID: <13E3F9DE-2603-473D-A483-132C52AA41BF@astro.su.se>


Dear all,

You are kindly invited to the licentiate thesis defense of Emir Karamehmetoglu to be held this Monday June 4th, 10-12 in FB42. The title is: "Looking for the high mass progenitors of stripped envelope supernovae". The opponent will be Poonam Chandra and the committee members will be Evan O’Connor and Michael Rutkowski. Please see the link from the Albanova agenda for the abstract and details. Looking forward to seeing you all there. 

Here is a link to the pdf of the licentiate thesis <https://www.dropbox.com/s/q96ntt0fx93babp/Emir_Licentiate.pdf?dl=0>. 

Kind regards,
Francesco/Jesper/Emir

Albanova Agenda:
https://www.albanova.se/event/licentiate-thesis-looking-for-the-high-mass-progenitors-of-stripped-envelope-supernovae/ <https://www.albanova.se/event/licentiate-thesis-looking-for-the-high-mass-progenitors-of-stripped-envelope-supernovae/>

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From evan.oconnor at astro.su.se  Mon Jun  4 14:11:16 2018
From: evan.oconnor at astro.su.se (Evan Patrick O'Connor)
Date: Mon, 4 Jun 2018 12:11:16 +0000
Subject: [Okc-wp4] Fw: Nordita Astrophysics Seminar Thu. June 7 @ 13:30
In-Reply-To: <E19FF50E-5B2F-448E-9025-01142AB811F5@su.se>
References: <E19FF50E-5B2F-448E-9025-01142AB811F5@su.se>
Message-ID: <1528114272578.37088@astro.su.se>

?Of interest for the EO group...

________________________________
From: Joonas Nättilä <joonas.nattila at su.se>
Sent: Monday, June 4, 2018 1:58 PM
To: people at nordita.org; alla at astro.su.se
Cc: Andrew W. Steiner
Subject: Nordita Astrophysics Seminar Thu. June 7 @ 13:30

Dear All,

The next Nordita Astrophysics Seminar will be on Thursday June 7 at 13:30 (room 112:028, Nordita South Building). Note the day since our usual Wednesday is a national holiday.



Speaker:
Andrew Steiner (Univ. Tennessee / Oak Ridge National Lab)

Title:
The Nature of Dense Matter from Multi-Messenger Observations of Neutron Stars

Abstract:
Constructing the most complete picture of the neutron star interior is (currently) only possible through the combined analysis of several data sets. We use Bayesian inference to combine neutron star observations, nuclear experiments, and nuclear theory. In this talk, I will begin by describing some of the methodology before presenting our predictions for neutron star tidal deformabilities and their relationship to GW170817. I will then go beyond the bulk thermodynamics of dense matter and show how our work is beginning to constrain the proton-to-neutron ratio and the nature of superfluidity in dense matter. Finally, I will describe how our results can be used as the input for more accurate simulations of neutron star mergers.

Welcome!

Add to calendar:   http://agenda.albanova.se/conferenceDisplay.py/ical?confId=6562


Cheers,
Joonas

---
Nordita Fellow
KTH Royal Institute of Technology and Stockholm University
Roslagstullsbacken 17, SE-10691 Stockholm, Sweden

http://natj.github.io

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From stephan.rosswog at astro.su.se  Tue Aug 14 14:35:19 2018
From: stephan.rosswog at astro.su.se (Stephan Rosswog)
Date: Tue, 14 Aug 2018 12:35:19 +0000
Subject: [Okc-wp4] 1st anniversary of GW/EM 170817
Message-ID: <1ED4E8B6-703C-43A7-B26F-5FE1E596B6BE@astro.su.se>

Dear all

as you may have realized, this Friday the first coincident discovery
of a neutron star merger in gravitational and electromagnetic waves
has its first anniversary.

To celebrate the first birthday (or just because it’s Friday) I suggest
to have some beer (and maybe a burger) at a Pub.
I suggest 18:00 at the Churchill Arms.

To have a rough idea how many people are interested, please fill in
 the following doodle:

https://doodle.com/poll/idgy82q8g4f6uts5

Please feel free to forward this to potentially interested people that
may not be on list.

 Cheers

Stephan

----------------------------------------------
Prof. Dr. Stephan Rosswog
Computational High-Energy Astrophysics

The Oskar Klein Centre for Cosmoparticle Physics
Department of Astronomy, Stockholm University
AlbaNova, Roslagstullbacken 21
SE-10691 Stockholm, Sweden

Email: stephan.rosswog at astro.su.se<mailto:stephan.rosswog at astro.su.se>
Tel.:     +46 (0)8 5537 8529
URL:   http://compact-merger.astro.su.se/

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From ftadd at astro.su.se  Tue Sep 11 15:32:40 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Tue, 11 Sep 2018 15:32:40 +0200
Subject: [Okc-wp4] EO meeting Sept. 13th
Message-ID: <BE9CFDBD-25D3-4DF3-90CF-DCAF6334F696@astro.su.se>

Hi all,

we restart with our EO meetings after the summer with Evan O’Connor
talking about: "Neutrino Transport Comparisons in Core-Collapse Supernovae"

Here the abstract:
Neutrino transport in both core-collapse supernovae and compact object mergers is crucial in order to capture the correct dynamical and chemical evolution of the matter.  In this talk I will present the results from two recent core-collapse supernova studies comparing neutrino transport in eight different codes with five different neutrino transport methods. I will also briefly show some results of neutrino transport in compact object mergers and the impact that different neutrino transport approximations can have on the chemical evolution.


Time & place : this Thursday (Sept. 13), at 13:00, KTH meeting room on the 5th floor

cheers

/Francesco


From ftadd at astro.su.se  Thu Sep 13 11:20:36 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 13 Sep 2018 11:20:36 +0200
Subject: [Okc-wp4] Reminder:  EO meeting Sept. 13th
In-Reply-To: <BE9CFDBD-25D3-4DF3-90CF-DCAF6334F696@astro.su.se>
References: <BE9CFDBD-25D3-4DF3-90CF-DCAF6334F696@astro.su.se>
Message-ID: <0653D957-2F8C-43E1-B77A-73BB59D5CDF8@astro.su.se>


TODAY!!

> On 11 Sep 2018, at 15:32, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> we restart with our EO meetings after the summer with Evan O’Connor
> talking about: "Neutrino Transport Comparisons in Core-Collapse Supernovae"
> 
> Here the abstract:
> Neutrino transport in both core-collapse supernovae and compact object mergers is crucial in order to capture the correct dynamical and chemical evolution of the matter.  In this talk I will present the results from two recent core-collapse supernova studies comparing neutrino transport in eight different codes with five different neutrino transport methods. I will also briefly show some results of neutrino transport in compact object mergers and the impact that different neutrino transport approximations can have on the chemical evolution.
> 
> 
> Time & place : this Thursday (Sept. 13), at 13:00, KTH meeting room on the 5th floor
> 
> cheers
> 
> /Francesco
> 
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list


From ftadd at astro.su.se  Tue Sep 25 12:07:34 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Tue, 25 Sep 2018 12:07:34 +0200
Subject: [Okc-wp4] EO meeting, Thursday 27th (13:00)
Message-ID: <7D483DEA-AA6C-4CD3-9C69-D700480279D2@astro.su.se>

Hi all,

two talks at our next EO meeting:


1) Christoffer Lundman will talk about: Prompt GRB emission from "deep" radiation mediated shocks

Abstract:
The mechanism that produces the prompt GRB emission is still unknown. One attractive scenario involves a variable central engine that produces shocks below the GRB photosphere. I will discuss recent work regarding the radiation produced by such "deep shocks." In particular, we've shown that the simplest shock scenario produces a smoothly broken power law spectrum with an exponential cut-off at high energies. I will also discuss possible ways of fitting such spectra to observations.

2) And I (Francesco Taddia) will present the results from two recent papers
on the peculiar supernovae iPTF14hls and iPTF15dtg:

on iPTF14hls:
https://arxiv.org/abs/1806.10001 <https://arxiv.org/abs/1806.10001>

on iPTF15dtg:
https://arxiv.org/abs/1806.10000 <https://arxiv.org/abs/1806.10000>

see you in the KTH meeting room, 5th floor.

cheers

/Francesco
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From ftadd at astro.su.se  Thu Sep 27 10:36:31 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 27 Sep 2018 10:36:31 +0200
Subject: [Okc-wp4] Reminder:  EO meeting, Thursday 27th (13:00)
In-Reply-To: <7D483DEA-AA6C-4CD3-9C69-D700480279D2@astro.su.se>
References: <7D483DEA-AA6C-4CD3-9C69-D700480279D2@astro.su.se>
Message-ID: <834BAC54-9A3D-4AC3-8397-1DE6D616E796@astro.su.se>

TODAY!

> On 25 Sep 2018, at 12:07, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> two talks at our next EO meeting:
> 
> 
> 1) Christoffer Lundman will talk about: Prompt GRB emission from "deep" radiation mediated shocks
> 
> Abstract:
> The mechanism that produces the prompt GRB emission is still unknown. One attractive scenario involves a variable central engine that produces shocks below the GRB photosphere. I will discuss recent work regarding the radiation produced by such "deep shocks." In particular, we've shown that the simplest shock scenario produces a smoothly broken power law spectrum with an exponential cut-off at high energies. I will also discuss possible ways of fitting such spectra to observations.
> 
> 2) And I (Francesco Taddia) will present the results from two recent papers
> on the peculiar supernovae iPTF14hls and iPTF15dtg:
> 
> on iPTF14hls:
> https://arxiv.org/abs/1806.10001 <https://arxiv.org/abs/1806.10001>
> 
> on iPTF15dtg:
> https://arxiv.org/abs/1806.10000 <https://arxiv.org/abs/1806.10000>
> 
> see you in the KTH meeting room, 5th floor.
> 
> cheers
> 
> /Francesco
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Mon Oct  8 13:32:23 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 8 Oct 2018 13:32:23 +0200
Subject: [Okc-wp4] EO meeting on Oct 11
Message-ID: <2E3C9785-0EA9-4793-A92A-20A4896908C7@astro.su.se>

Dear all,

our next speaker at the EO meeting (oct 11, 13:00, @KTH meeting room on the 5th floor),
will be André da SIlva Schneider. Below the info on his talk:

%%%%%%%%%%%%%
Title: "Equation of State Effects on Core-collapse Supernovae"

Abstract: 

In this talk I present a method to compute the equation of state (EOS) of dense matter for astrophysical simulations. 
I discuss how current uncertainties in the parameters that determine the EOS affect the outcome of a core-collapse supernova simulation. 

%%%%%%%%%%%%%

cheers

/Francesco
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From ftadd at astro.su.se  Thu Oct 11 09:21:29 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 11 Oct 2018 09:21:29 +0200
Subject: [Okc-wp4] Reminder:  EO meeting on Oct 11
In-Reply-To: <2E3C9785-0EA9-4793-A92A-20A4896908C7@astro.su.se>
References: <2E3C9785-0EA9-4793-A92A-20A4896908C7@astro.su.se>
Message-ID: <89049196-2AA5-4C91-B814-1F59FD5D92FD@astro.su.se>


TODAY!!


> On 8 Oct 2018, at 13:32, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Dear all,
> 
> our next speaker at the EO meeting (oct 11, 13:00, @KTH meeting room on the 5th floor),
> will be André da SIlva Schneider. Below the info on his talk:
> 
> %%%%%%%%%%%%%
> Title: "Equation of State Effects on Core-collapse Supernovae"
> 
> Abstract: 
> 
> In this talk I present a method to compute the equation of state (EOS) of dense matter for astrophysical simulations. 
> I discuss how current uncertainties in the parameters that determine the EOS affect the outcome of a core-collapse supernova simulation. 
> 
> %%%%%%%%%%%%%
> 
> cheers
> 
> /Francesco
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Mon Oct 22 17:12:50 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 22 Oct 2018 17:12:50 +0200
Subject: [Okc-wp4] EO meeting Oct 25
Message-ID: <083276D2-9AE3-49F5-BE42-9FB41F236D77@astro.su.se>

Dear all,

on Thursday (Oct 25, 13:00-14:00, KTH meeting room on the 5th floor) we will have our next EO meeting,
where Francesca Capel will give the following talk:

Title: A hierarchical model for the sources of ultra-high energy cosmic rays (UHECR)

Abstract:
The study of UHECR is challenged by both the rarity of events and the difficulty in modelling their production, propagation and detection. I will present a Bayesian hierarchical model which enables a joint fit of the UHECR energy spectrum and arrival directions with a physical model of UHECR phenomenology. In this way, possible associations with candidate source catalogs can be assessed in a physically and statistically principled manner. Results from the application of the model to data from the Pierre Auger Observatory will also be shown.


cheers

/Francesco
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From ftadd at astro.su.se  Thu Oct 25 09:37:21 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 25 Oct 2018 09:37:21 +0200
Subject: [Okc-wp4] Reminder:  EO meeting Oct 25
In-Reply-To: <083276D2-9AE3-49F5-BE42-9FB41F236D77@astro.su.se>
References: <083276D2-9AE3-49F5-BE42-9FB41F236D77@astro.su.se>
Message-ID: <D3668ABC-B90B-4295-AD36-F4D23BCD0C19@astro.su.se>

TODAY!!!

> On 22 Oct 2018, at 17:12, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Dear all,
> 
> on Thursday (Oct 25, 13:00-14:00, KTH meeting room on the 5th floor) we will have our next EO meeting,
> where Francesca Capel will give the following talk:
> 
> Title: A hierarchical model for the sources of ultra-high energy cosmic rays (UHECR)
> 
> Abstract:
> The study of UHECR is challenged by both the rarity of events and the difficulty in modelling their production, propagation and detection. I will present a Bayesian hierarchical model which enables a joint fit of the UHECR energy spectrum and arrival directions with a physical model of UHECR phenomenology. In this way, possible associations with candidate source catalogs can be assessed in a physically and statistically principled manner. Results from the application of the model to data from the Pierre Auger Observatory will also be shown.
> 
> 
> cheers
> 
> /Francesco
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list

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From ftadd at astro.su.se  Mon Nov  5 09:06:32 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 5 Nov 2018 09:06:32 +0100
Subject: [Okc-wp4] Upcoming EO meetings
Message-ID: <A142CD53-ADBE-4018-974A-3206E6AD8877@astro.su.se>

Hi all,

here the speakers and the dates for the upcoming EO meetings, more info on the next one (this thursday) later today,

cheers

/Francesco

Nov 08:  Christian Setzer
Nov 22:  David Kaplan
Dec 06:  Ragnhild Lunnan

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From ftadd at astro.su.se  Mon Nov  5 13:52:24 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 5 Nov 2018 13:52:24 +0100
Subject: [Okc-wp4] EO meeting on Nov 8
Message-ID: <E273E48B-A712-4C6F-B2E8-EE5374E94FAB@astro.su.se>

Hi all,

this Thursday at 13:00 (@KTH meeting room on the 5th floor),
Christian Setzer will talk about our ability to serendipitously detect both binary neutron star
merger and neutron star black hole merger kilonovae with the LSST. 

see you there,

cheers

/Francesco

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From ftadd at astro.su.se  Thu Nov  8 11:37:00 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 8 Nov 2018 11:37:00 +0100
Subject: [Okc-wp4] Reminder: EO meeting on Nov 8
In-Reply-To: <E273E48B-A712-4C6F-B2E8-EE5374E94FAB@astro.su.se>
References: <E273E48B-A712-4C6F-B2E8-EE5374E94FAB@astro.su.se>
Message-ID: <31BD20AA-4010-4504-8FD1-968D3CCC43B0@astro.su.se>

Today!

> On 5 Nov 2018, at 13:52, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Hi all,
> 
> this Thursday at 13:00 (@KTH meeting room on the 5th floor),
> Christian Setzer will talk about our ability to serendipitously detect both binary neutron star
> merger and neutron star black hole merger kilonovae with the LSST. 
> 
> see you there,
> 
> cheers
> 
> /Francesco
> 

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From ftadd at astro.su.se  Mon Nov 19 17:12:13 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Mon, 19 Nov 2018 17:12:13 +0100
Subject: [Okc-wp4] EO meeting on Nov 22th
Message-ID: <F151D2FF-C534-426C-8B75-14C6A57E66F6@astro.su.se>

Dear all,

our next EO meeting will be this Thursday at 13:00 (5th floor KTH meeting room).

David Kaplan will give the following talk:

Title: Probing Stellar Evolution, Dynamics, and Fundamental Physics with
Millisecond Pulsar Binaries

Abstract:  Pulsars are the ultra-dense rotating remnants of massive stars that
exploded at the ends of their lives.  Millisecond pulsars are normal
pulsars that have been "recycled" and been brought back from the dead
by a binary companion.  I will discuss new results on binary systems
consisting of millisecond pulsars and other stars.  Drawing upon
recent results, I will explore areas where these binaries help give
independent constraints on the nature, properties, and evolution of
compact binary systems.  I will focus on what can be learned from
"fast" millisecond pulsar binaries: those systems that are moving
across the sky quickly enough that the Shklovskii effect significantly
affects their spin-down behavior.  In some of these systems anomalous
spin-down behavior has led to clues about their nature, formation, and
evolution.


see you there!

cheers

/Francesco

From andre.schneider at astro.su.se  Tue Nov 20 12:29:46 2018
From: andre.schneider at astro.su.se (Andre Schneider)
Date: Tue, 20 Nov 2018 11:29:46 +0000
Subject: [Okc-wp4]  EO meeting on Nov 22th
Message-ID: <87e3a3f0d971439a802e39b0bfbca527@astro.su.se>

our next EO meeting will be this Thursday at 13:00 (5th floor KTH meeting room).
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From ftadd at astro.su.se  Thu Nov 22 08:56:15 2018
From: ftadd at astro.su.se (Francesco Taddia)
Date: Thu, 22 Nov 2018 08:56:15 +0100
Subject: [Okc-wp4] Reminder:  EO meeting on Nov 22th
In-Reply-To: <F151D2FF-C534-426C-8B75-14C6A57E66F6@astro.su.se>
References: <F151D2FF-C534-426C-8B75-14C6A57E66F6@astro.su.se>
Message-ID: <ECA5894C-9E66-42B3-836B-939AE43E9A1D@astro.su.se>

Today!

> On 19 Nov 2018, at 17:12, Francesco Taddia <ftadd at astro.su.se> wrote:
> 
> Dear all,
> 
> our next EO meeting will be this Thursday at 13:00 (5th floor KTH meeting room).
> 
> David Kaplan will give the following talk:
> 
> Title: Probing Stellar Evolution, Dynamics, and Fundamental Physics with
> Millisecond Pulsar Binaries
> 
> Abstract:  Pulsars are the ultra-dense rotating remnants of massive stars that
> exploded at the ends of their lives.  Millisecond pulsars are normal
> pulsars that have been "recycled" and been brought back from the dead
> by a binary companion.  I will discuss new results on binary systems
> consisting of millisecond pulsars and other stars.  Drawing upon
> recent results, I will explore areas where these binaries help give
> independent constraints on the nature, properties, and evolution of
> compact binary systems.  I will focus on what can be learned from
> "fast" millisecond pulsar binaries: those systems that are moving
> across the sky quickly enough that the Shklovskii effect significantly
> affects their spin-down behavior.  In some of these systems anomalous
> spin-down behavior has led to clues about their nature, formation, and
> evolution.
> 
> 
> see you there!
> 
> cheers
> 
> /Francesco
> 
> -------------------------------------------------
> okc-wp4 at albanova.se mailing list


From mattia.bulla at fysik.su.se  Fri Nov 23 11:52:44 2018
From: mattia.bulla at fysik.su.se (Mattia Bulla)
Date: Fri, 23 Nov 2018 10:52:44 +0000
Subject: [Okc-wp4] Joint SN meeting 2018-11-28
Message-ID: <8F1F156D-B65A-4209-8320-6B8544E2E8A7@fysik.su.se>

Dear all,

our next Joint SN meeting will be on Wednesday, Nov 28 at 10:30 (A5:1003, 5th floor KTH room).

Our speaker is Joseph K. Swiggum who will be visiting the Astronomy department next week. Title and abstract follow below.

I am sending the invitation to both the “Joint SN meeting” and “EO meeting” mailing lists, apologise if you receive this more than once.


Title: Constructing a gravitational wave detector with pulsar surveys

Abstract: Pulsar timing array (PTA) experiments like the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) aim to detect correlated signatures of low frequency gravitational waves in millisecond pulsar (MSP) timing data. Adding four MSPs to the array each year is expected to provide adequate sensitivity to detect an isotropic, stochastic gravitational wave background within the next decade. Current pulsar surveys like the Green Bank North Celestial Cap (GBNCC) survey continue to discover bright MSPs and rapidly assess their suitability for PTAs; these discoveries also improve our understanding of the underlying MSP population to inform future PTA sensitivity predictions.


Best,
Mattia

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From mattia.bulla at fysik.su.se  Wed Nov 28 06:48:30 2018
From: mattia.bulla at fysik.su.se (Mattia Bulla)
Date: Wed, 28 Nov 2018 05:48:30 +0000
Subject: [Okc-wp4] Joint SN meeting 2018-11-28
Message-ID: <e38fbc45-8094-4c5c-8ea5-aa74aff70360@email.android.com>

Dear all,

this is a kind reminder of today's talk by Joseph Swiggum. 10.30, A5:1003.

Best,
Mattia


On Nov 23, 2018 11:52, Mattia Bulla <mattia.bulla at fysik.su.se> wrote:
Dear all,

our next Joint SN meeting will be on Wednesday, Nov 28 at 10:30 (A5:1003, 5th floor KTH room).

Our speaker is Joseph K. Swiggum who will be visiting the Astronomy department next week. Title and abstract follow below.

I am sending the invitation to both the “Joint SN meeting” and “EO meeting” mailing lists, apologise if you receive this more than once.


Title: Constructing a gravitational wave detector with pulsar surveys

Abstract: Pulsar timing array (PTA) experiments like the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) aim to detect correlated signatures of low frequency gravitational waves in millisecond pulsar (MSP) timing data. Adding four MSPs to the array each year is expected to provide adequate sensitivity to detect an isotropic, stochastic gravitational wave background within the next decade. Current pulsar surveys like the Green Bank North Celestial Cap (GBNCC) survey continue to discover bright MSPs and rapidly assess their suitability for PTAs; these discoveries also improve our understanding of the underlying MSP population to inform future PTA sensitivity predictions.


Best,
Mattia


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From andre.schneider at astro.su.se  Tue Dec  4 10:15:04 2018
From: andre.schneider at astro.su.se (Andre Schneider)
Date: Tue, 4 Dec 2018 09:15:04 +0000
Subject: [Okc-wp4] EO meeting on Dec 6
Message-ID: <ba53ab691d424b93b38c01618b529ac5@astro.su.se>



Dear all,

our next speaker at the EO meeting (Dec 6, 13:00, @KTH meeting room on the 5th floor), will be Ragnhild Lunnan. Below is the info on her talk.



Rapidly Evolving Transients in the ZTF Era


Large-scale untargeted optical surveys are discovering many new types of transient phenomena beyond the standard Type Ia and core-collapse supernova paradigm. One relatively unexplored part of parameter space is transients with shorter timescales (~days rather than ~weeks), as traditional supernova searches were not particularly sensitive to such events. Analysis from the Pan-STARRS Medium Deep Survey suggests such transients constitute as much as 4-7% of the core-collapse supernova rate, however. In this talk, I will review previous work on rapidly evolving transients as well as discuss some recent, interesting events from iPTF and ZTF.


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From andre.schneider at astro.su.se  Thu Dec  6 09:59:06 2018
From: andre.schneider at astro.su.se (Andre Schneider)
Date: Thu, 6 Dec 2018 08:59:06 +0000
Subject: [Okc-wp4] Fw: EO meeting on Dec 6
In-Reply-To: <ba53ab691d424b93b38c01618b529ac5@astro.su.se>
References: <ba53ab691d424b93b38c01618b529ac5@astro.su.se>
Message-ID: <02da3983abc047cb8001dbbc73094c8b@astro.su.se>



Reminded of our EO meeting today at 13:00.


________________________________
From: Okc-wp4-at-fysik.su.se <okc-wp4-at-fysik.su.se-bounces at lists.su.se> on behalf of Andre Schneider <andre.schneider at astro.su.se>
Sent: Tuesday, December 4, 2018 10:15 AM
To: okc-wp4-at-fysik.su.se at lists.su.se
Subject: [Okc-wp4] EO meeting on Dec 6



Dear all,

our next speaker at the EO meeting (Dec 6, 13:00, @KTH meeting room on the 5th floor), will be Ragnhild Lunnan. Below is the info on her talk.



Rapidly Evolving Transients in the ZTF Era


Large-scale untargeted optical surveys are discovering many new types of transient phenomena beyond the standard Type Ia and core-collapse supernova paradigm. One relatively unexplored part of parameter space is transients with shorter timescales (~days rather than ~weeks), as traditional supernova searches were not particularly sensitive to such events. Analysis from the Pan-STARRS Medium Deep Survey suggests such transients constitute as much as 4-7% of the core-collapse supernova rate, however. In this talk, I will review previous work on rapidly evolving transients as well as discuss some recent, interesting events from iPTF and ZTF.


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