Please read these instructions before posting any event on Fermilab Indico
Focus on:
All days
11 Sep 2017
12 Sep 2017
13 Sep 2017
14 Sep 2017
15 Sep 2017
16 Sep 2017
17 Sep 2017
18 Sep 2017
19 Sep 2017
20 Sep 2017
21 Sep 2017
22 Sep 2017
23 Sep 2017
24 Sep 2017
25 Sep 2017
26 Sep 2017
27 Sep 2017
28 Sep 2017
29 Sep 2017
30 Sep 2017
1 Oct 2017
2 Oct 2017
3 Oct 2017
4 Oct 2017
5 Oct 2017
6 Oct 2017
Indico style
Indico style - inline minutes
Indico style - numbered
Indico style - numbered + minutes
Indico Weeks View
Back to Conference View
Choose Timezone
Use the event/category timezone
Specify a timezone
Africa/Abidjan
Africa/Accra
Africa/Addis_Ababa
Africa/Algiers
Africa/Asmara
Africa/Bamako
Africa/Bangui
Africa/Banjul
Africa/Bissau
Africa/Blantyre
Africa/Brazzaville
Africa/Bujumbura
Africa/Cairo
Africa/Casablanca
Africa/Ceuta
Africa/Conakry
Africa/Dakar
Africa/Dar_es_Salaam
Africa/Djibouti
Africa/Douala
Africa/El_Aaiun
Africa/Freetown
Africa/Gaborone
Africa/Harare
Africa/Johannesburg
Africa/Juba
Africa/Kampala
Africa/Khartoum
Africa/Kigali
Africa/Kinshasa
Africa/Lagos
Africa/Libreville
Africa/Lome
Africa/Luanda
Africa/Lubumbashi
Africa/Lusaka
Africa/Malabo
Africa/Maputo
Africa/Maseru
Africa/Mbabane
Africa/Mogadishu
Africa/Monrovia
Africa/Nairobi
Africa/Ndjamena
Africa/Niamey
Africa/Nouakchott
Africa/Ouagadougou
Africa/Porto-Novo
Africa/Sao_Tome
Africa/Tripoli
Africa/Tunis
Africa/Windhoek
America/Adak
America/Anchorage
America/Anguilla
America/Antigua
America/Araguaina
America/Argentina/Buenos_Aires
America/Argentina/Catamarca
America/Argentina/Cordoba
America/Argentina/Jujuy
America/Argentina/La_Rioja
America/Argentina/Mendoza
America/Argentina/Rio_Gallegos
America/Argentina/Salta
America/Argentina/San_Juan
America/Argentina/San_Luis
America/Argentina/Tucuman
America/Argentina/Ushuaia
America/Aruba
America/Asuncion
America/Atikokan
America/Bahia
America/Bahia_Banderas
America/Barbados
America/Belem
America/Belize
America/Blanc-Sablon
America/Boa_Vista
America/Bogota
America/Boise
America/Cambridge_Bay
America/Campo_Grande
America/Cancun
America/Caracas
America/Cayenne
America/Cayman
America/Chicago
America/Chihuahua
America/Costa_Rica
America/Creston
America/Cuiaba
America/Curacao
America/Danmarkshavn
America/Dawson
America/Dawson_Creek
America/Denver
America/Detroit
America/Dominica
America/Edmonton
America/Eirunepe
America/El_Salvador
America/Fort_Nelson
America/Fortaleza
America/Glace_Bay
America/Goose_Bay
America/Grand_Turk
America/Grenada
America/Guadeloupe
America/Guatemala
America/Guayaquil
America/Guyana
America/Halifax
America/Havana
America/Hermosillo
America/Indiana/Indianapolis
America/Indiana/Knox
America/Indiana/Marengo
America/Indiana/Petersburg
America/Indiana/Tell_City
America/Indiana/Vevay
America/Indiana/Vincennes
America/Indiana/Winamac
America/Inuvik
America/Iqaluit
America/Jamaica
America/Juneau
America/Kentucky/Louisville
America/Kentucky/Monticello
America/Kralendijk
America/La_Paz
America/Lima
America/Los_Angeles
America/Lower_Princes
America/Maceio
America/Managua
America/Manaus
America/Marigot
America/Martinique
America/Matamoros
America/Mazatlan
America/Menominee
America/Merida
America/Metlakatla
America/Mexico_City
America/Miquelon
America/Moncton
America/Monterrey
America/Montevideo
America/Montserrat
America/Nassau
America/New_York
America/Nipigon
America/Nome
America/Noronha
America/North_Dakota/Beulah
America/North_Dakota/Center
America/North_Dakota/New_Salem
America/Nuuk
America/Ojinaga
America/Panama
America/Pangnirtung
America/Paramaribo
America/Phoenix
America/Port-au-Prince
America/Port_of_Spain
America/Porto_Velho
America/Puerto_Rico
America/Punta_Arenas
America/Rainy_River
America/Rankin_Inlet
America/Recife
America/Regina
America/Resolute
America/Rio_Branco
America/Santarem
America/Santiago
America/Santo_Domingo
America/Sao_Paulo
America/Scoresbysund
America/Sitka
America/St_Barthelemy
America/St_Johns
America/St_Kitts
America/St_Lucia
America/St_Thomas
America/St_Vincent
America/Swift_Current
America/Tegucigalpa
America/Thule
America/Thunder_Bay
America/Tijuana
America/Toronto
America/Tortola
America/Vancouver
America/Whitehorse
America/Winnipeg
America/Yakutat
America/Yellowknife
Antarctica/Casey
Antarctica/Davis
Antarctica/DumontDUrville
Antarctica/Macquarie
Antarctica/Mawson
Antarctica/McMurdo
Antarctica/Palmer
Antarctica/Rothera
Antarctica/Syowa
Antarctica/Troll
Antarctica/Vostok
Arctic/Longyearbyen
Asia/Aden
Asia/Almaty
Asia/Amman
Asia/Anadyr
Asia/Aqtau
Asia/Aqtobe
Asia/Ashgabat
Asia/Atyrau
Asia/Baghdad
Asia/Bahrain
Asia/Baku
Asia/Bangkok
Asia/Barnaul
Asia/Beirut
Asia/Bishkek
Asia/Brunei
Asia/Chita
Asia/Choibalsan
Asia/Colombo
Asia/Damascus
Asia/Dhaka
Asia/Dili
Asia/Dubai
Asia/Dushanbe
Asia/Famagusta
Asia/Gaza
Asia/Hebron
Asia/Ho_Chi_Minh
Asia/Hong_Kong
Asia/Hovd
Asia/Irkutsk
Asia/Jakarta
Asia/Jayapura
Asia/Jerusalem
Asia/Kabul
Asia/Kamchatka
Asia/Karachi
Asia/Kathmandu
Asia/Khandyga
Asia/Kolkata
Asia/Krasnoyarsk
Asia/Kuala_Lumpur
Asia/Kuching
Asia/Kuwait
Asia/Macau
Asia/Magadan
Asia/Makassar
Asia/Manila
Asia/Muscat
Asia/Nicosia
Asia/Novokuznetsk
Asia/Novosibirsk
Asia/Omsk
Asia/Oral
Asia/Phnom_Penh
Asia/Pontianak
Asia/Pyongyang
Asia/Qatar
Asia/Qostanay
Asia/Qyzylorda
Asia/Riyadh
Asia/Sakhalin
Asia/Samarkand
Asia/Seoul
Asia/Shanghai
Asia/Singapore
Asia/Srednekolymsk
Asia/Taipei
Asia/Tashkent
Asia/Tbilisi
Asia/Tehran
Asia/Thimphu
Asia/Tokyo
Asia/Tomsk
Asia/Ulaanbaatar
Asia/Urumqi
Asia/Ust-Nera
Asia/Vientiane
Asia/Vladivostok
Asia/Yakutsk
Asia/Yangon
Asia/Yekaterinburg
Asia/Yerevan
Atlantic/Azores
Atlantic/Bermuda
Atlantic/Canary
Atlantic/Cape_Verde
Atlantic/Faroe
Atlantic/Madeira
Atlantic/Reykjavik
Atlantic/South_Georgia
Atlantic/St_Helena
Atlantic/Stanley
Australia/Adelaide
Australia/Brisbane
Australia/Broken_Hill
Australia/Darwin
Australia/Eucla
Australia/Hobart
Australia/Lindeman
Australia/Lord_Howe
Australia/Melbourne
Australia/Perth
Australia/Sydney
Canada/Atlantic
Canada/Central
Canada/Eastern
Canada/Mountain
Canada/Newfoundland
Canada/Pacific
Europe/Amsterdam
Europe/Andorra
Europe/Astrakhan
Europe/Athens
Europe/Belgrade
Europe/Berlin
Europe/Bratislava
Europe/Brussels
Europe/Bucharest
Europe/Budapest
Europe/Busingen
Europe/Chisinau
Europe/Copenhagen
Europe/Dublin
Europe/Gibraltar
Europe/Guernsey
Europe/Helsinki
Europe/Isle_of_Man
Europe/Istanbul
Europe/Jersey
Europe/Kaliningrad
Europe/Kiev
Europe/Kirov
Europe/Lisbon
Europe/Ljubljana
Europe/London
Europe/Luxembourg
Europe/Madrid
Europe/Malta
Europe/Mariehamn
Europe/Minsk
Europe/Monaco
Europe/Moscow
Europe/Oslo
Europe/Paris
Europe/Podgorica
Europe/Prague
Europe/Riga
Europe/Rome
Europe/Samara
Europe/San_Marino
Europe/Sarajevo
Europe/Saratov
Europe/Simferopol
Europe/Skopje
Europe/Sofia
Europe/Stockholm
Europe/Tallinn
Europe/Tirane
Europe/Ulyanovsk
Europe/Uzhgorod
Europe/Vaduz
Europe/Vatican
Europe/Vienna
Europe/Vilnius
Europe/Volgograd
Europe/Warsaw
Europe/Zagreb
Europe/Zaporozhye
Europe/Zurich
GMT
Indian/Antananarivo
Indian/Chagos
Indian/Christmas
Indian/Cocos
Indian/Comoro
Indian/Kerguelen
Indian/Mahe
Indian/Maldives
Indian/Mauritius
Indian/Mayotte
Indian/Reunion
Pacific/Apia
Pacific/Auckland
Pacific/Bougainville
Pacific/Chatham
Pacific/Chuuk
Pacific/Easter
Pacific/Efate
Pacific/Fakaofo
Pacific/Fiji
Pacific/Funafuti
Pacific/Galapagos
Pacific/Gambier
Pacific/Guadalcanal
Pacific/Guam
Pacific/Honolulu
Pacific/Kanton
Pacific/Kiritimati
Pacific/Kosrae
Pacific/Kwajalein
Pacific/Majuro
Pacific/Marquesas
Pacific/Midway
Pacific/Nauru
Pacific/Niue
Pacific/Norfolk
Pacific/Noumea
Pacific/Pago_Pago
Pacific/Palau
Pacific/Pitcairn
Pacific/Pohnpei
Pacific/Port_Moresby
Pacific/Rarotonga
Pacific/Saipan
Pacific/Tahiti
Pacific/Tarawa
Pacific/Tongatapu
Pacific/Wake
Pacific/Wallis
US/Alaska
US/Arizona
US/Central
US/Eastern
US/Hawaii
US/Mountain
US/Pacific
UTC
Save
Europe/Paris
English (United Kingdom)
English (United Kingdom)
English (United States)
Español (España)
Français (France)
Polski (Polska)
Português (Brasil)
Türkçe (Türkiye)
Монгол (Монгол)
Українська (Україна)
中文 (中国)
Login
Dark Energy and Modified-Gravity cosmologies: DARKMOD
from
Monday, 11 September 2017 (09:30)
to
Friday, 6 October 2017 (17:00)
Monday, 11 September 2017
09:30
Betoule: "SNeIa, constraints on cosmology"
Betoule: "SNeIa, constraints on cosmology"
09:30 - 11:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Blanchard: Formation of large-scale structures, clusters of galaxies
Blanchard: Formation of large-scale structures, clusters of galaxies
14:00 - 15:30
16:00
Langlois: Introduction to modified gravity theories
Langlois: Introduction to modified gravity theories
16:00 - 17:30
Tuesday, 12 September 2017
09:00
Blanchard: Formation of large-scale structures, clusters of galaxies
Blanchard: Formation of large-scale structures, clusters of galaxies
09:00 - 10:30
11:00
Rich: "BAO - Lyman-alpha, constraints on cosmology"
Rich: "BAO - Lyman-alpha, constraints on cosmology"
11:00 - 12:30
13:00
lunch
lunch
13:00 - 14:15
14:15
Betoule: "SNeIa, constraints on cosmology"
Betoule: "SNeIa, constraints on cosmology"
14:15 - 15:45
16:15
Discussion: "Background versus perturbation constraints on models"
Discussion: "Background versus perturbation constraints on models"
16:15 - 17:15
Wednesday, 13 September 2017
10:00
Langlois: Introduction to modified gravity theories
Langlois: Introduction to modified gravity theories
10:00 - 11:30
12:30
lunch
lunch
12:30 - 14:00
14:00
Kilbinger: Weak lensing
Kilbinger: Weak lensing
14:00 - 15:30
16:00
Burtin: Redshift-space distortions
Burtin: Redshift-space distortions
16:00 - 17:00
17:00
Discussion: "Which observables to detect DE or MG ?"
Discussion: "Which observables to detect DE or MG ?"
17:00 - 18:00
Thursday, 14 September 2017
10:00
Kilbinger: Weak lensing
Kilbinger: Weak lensing
10:00 - 11:30
12:30
lunch
lunch
12:30 - 14:00
14:00
Rich: "BAO - Lyman-alpha, constraints on cosmology"
Rich: "BAO - Lyman-alpha, constraints on cosmology"
14:00 - 15:30
16:00
Langlois: Introduction to modified gravity theories
Langlois: Introduction to modified gravity theories
16:00 - 17:30
17:30
"Linear versus non-linear scales"
"Linear versus non-linear scales"
17:30 - 18:30
Friday, 15 September 2017
09:30
Kilbinger: weak lensing
Kilbinger: weak lensing
09:30 - 11:00
11:30
Mina: dark matter
Mina: dark matter
11:30 - 11:50
12:30
lunch
lunch
12:30 - 14:00
Saturday, 16 September 2017
Sunday, 17 September 2017
Monday, 18 September 2017
11:00
Tolley: Massive gravity
Tolley: Massive gravity
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Vernizzi: Effective Field Theory of Dark Energy
Vernizzi: Effective Field Theory of Dark Energy
14:00 - 15:00
Tuesday, 19 September 2017
11:00
Tolley: Massive gravity
Tolley: Massive gravity
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Vernizzi: Effective Field Theory of Dark Energy
Vernizzi: Effective Field Theory of Dark Energy
14:00 - 15:00
15:30
Senatore:
Senatore:
15:30 - 16:30
Wednesday, 20 September 2017
11:00
Tolley: Massive gravity
Tolley: Massive gravity
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Vernizzi: Effective Field Theory of Dark Energy
Vernizzi: Effective Field Theory of Dark Energy
14:00 - 15:00
Thursday, 21 September 2017
11:00
Tolley: Massive gravity
Tolley: Massive gravity
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Vernizzi: Effective Field Theory of Dark Energy
Vernizzi: Effective Field Theory of Dark Energy
14:00 - 15:00
15:00
Discussion: Constraints on Galileon models and other scenarios
Discussion: Constraints on Galileon models and other scenarios
15:00 - 16:00
16:00
Happy hour: beer, wine and crisps
Happy hour: beer, wine and crisps
16:00 - 17:00
Friday, 22 September 2017
11:00
Tolley: Massive gravity
Tolley: Massive gravity
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Vernizzi: Effective Field Theory of Dark Energy
Vernizzi: Effective Field Theory of Dark Energy
14:00 - 15:00
Saturday, 23 September 2017
Sunday, 24 September 2017
Monday, 25 September 2017
09:30
Creminelli: "Relaxation of the Cosmological Constant"
Creminelli: "Relaxation of the Cosmological Constant"
09:30 - 10:05
10:05
Tolley: "Positivity Bounds on Effective Field Theories of Gravity"
Tolley: "Positivity Bounds on Effective Field Theories of Gravity"
10:05 - 10:40
I will discuss recently developed positivity bounds for the scattering amplitudes of massive particles of any spin following from unitarity, Lorentz invariance and Analyticity and how these can be used to constrain various EFTs of gravity.
10:40
coffee
coffee
10:40 - 11:10
11:10
Bellini: "Towards a unified description of theories with a single scalar degree of freedom"
Bellini: "Towards a unified description of theories with a single scalar degree of freedom"
11:10 - 11:35
Models propagating a single extra degree of freedom are very popular as Dark Energy candidates. Examples are Scalar-Tensor, Vector-Tensor, and bimetric theories of gravity. Despite their common properties, these theories are usually described in different frameworks. I will show a method to construct general parametrizations to describe the linear dynamics of all these models. I will present the results in a unified formalism, and discuss under what circumstances it is possible to have a unified description for all these theories.
11:35
Vernizzi: "More on the Effective Theory of Dark Energy"
Vernizzi: "More on the Effective Theory of Dark Energy"
11:35 - 12:10
12:10
Kennedy: "Reconstructing Horndeski models from the effective field theory of dark energy"
Kennedy: "Reconstructing Horndeski models from the effective field theory of dark energy"
12:10 - 12:30
With the next generation of cosmological surveys about to commence, it is important to understand how one can use the information obtained from such surveys to constrain the space of dark energy and modified gravity theories. The effective field theory (EFT) of dark energy has proven to be a useful approach in this regard, allowing an efficient exploration of the parameter space. However, in order to gain a deeper understanding of the mechanism underlying cosmic acceleration one would like to interpret constraints on the EFT parameters in terms of fundamental covariant theories. In this talk I will discuss a method to reconstruct the class of covariant Horndeski theories that reproduce the same background dynamics and linear perturbations as a given EFT action. I will then present a number of examples and applications. The work was done in collaboration with Lucas Lombriser and Andy Taylor.
12:30
lunch
lunch
12:30 - 14:00
14:00
Khosravi: "Uber-Gravity and H0 tension"
Khosravi: "Uber-Gravity and H0 tension"
14:00 - 14:35
Recently, the idea of taking ensemble average over gravity models has been introduced. Based on this idea, we study the ensemble average over (effectively) all the gravity models dubbing the name ubergravity.
14:35
Cespedes: "Detecting modified gravity using B modes experiment"
Cespedes: "Detecting modified gravity using B modes experiment"
14:35 - 14:55
In this talk We will discuss the effects that a modified sector tensor can produce on the polarisation CMB power spectra. Alternative theories of gravity can give the graviton a mass but also modify the dispersion relation of the gravitational waves. by A mass for the graviton can affect the large angular scales and in general a modified dispersion relation could change the position of the acoustic peaks. These effect modifies either the CMB power spectrum and bispectrum, with respect to the canonical case. Thus given the precision of the CMB experiments, if detected, primordial gravitational waves can help to constraint gravity at a much higher accuracy.
14:55
Winther: "COLA with scale-dependent growth"
Winther: "COLA with scale-dependent growth"
14:55 - 15:20
N-body simulations is the main method we have to accurately compute observables in the non-linear regime of structure formation. Such simulations are too computationally expensive for many purposes, for example when one needs to generate large ensembles of galaxy mocks to model observables and their covariances for future surveys. Over the last few years a wide range of approximate methods for simulating structure formation have been proposed. I will first present a fast approximate method for including screening in numerical simulations of modified gravity theories and then show how one can extend the COmoving-Lagrangian-Acceleration (COLA) method to general models where the growth-rate is scale-dependent. These two methods can be combined and leads to a very fast method, often O(100) times faster than N-body, to compute clustering observables accurate down to fairly non-linear scales for a large class of models. Another application of the scale-dependent COLA method is that it allows for a simple way of including the effects of massive neutrinos on structure formation. The numerical code developed for this purpose is made available to the public and comes with several models already implemented.
15:20
Ebrahimi: "Clustering of Cold Dynamical Dark Energy Models"
Ebrahimi: "Clustering of Cold Dynamical Dark Energy Models"
15:20 - 15:40
The nature of dark energy can be investigated not only by equation of state but also through clustering and sound speed. In this research, we examine clustering of some dynamical dark energy models namely, power-law (PL), Chavelier-Polarski-Linder (CPL) and Feng-Shen-Li (FSL). We will go beyond zero-order and Free parameter of models constraints by using current available data including Planck DR2, Baryonic Acoustic Oscillation (BAO) and Supernovae type Ia (SNIa) observation and Hubble space telescope (HST). We investigate that PL as early dark energy has different behavior rather than semi-LCDM models such as rapid potential changes, higher matter density contrast due to crossing LCDM equation of state and matter behavior at early universe. We quantify the importance of uncoupled dark energy clustering, PL exhibits strong clustering with δP L > 0 which can grow faster than δm and semi-LCDM models produce void of dark energy with powerless amplitude around 10−12. In the linear regime, density contrast, growth rate index f(σ8) and gravitational potential computed. Furthermore, temperature anisotropy and matter power spectrum by modification of CAMB for dynamical models obtained and ISW effect. PL shows more ISW effect, more value for matter power spectrum at large scale around k=0.01.Tension between HST and CMB for H0 disappears for all models.
15:40
coffee
coffee
15:40 - 16:10
16:10
Naik: Simulating Milky Way-like galaxies under f(R) gravity
Naik: Simulating Milky Way-like galaxies under f(R) gravity
16:10 - 16:30
There is a growing body of work utilising N-body simulations with alternative gravity theories, but simulations at a galactic scale remain a relatively unexplored area. In this work, we present the first simulated galaxy rotation curves under f(R) gravity to our knowledge. The f(R) gravity solver MG-GADGET (Puchwein et al. 2013) is employed statically on pre-simulated spiral galaxies, leading to solutions for the rotation curves and screening radii under HuSawicki f(R) gravity. It is shown that under certain parameter regimes, the so-called 'fifth force' yields observable signatures, which can be exploited to constrain departures from classical gravity.
16:30
Armengaud: Ultra-light scalar Dark Matter probed with the Lyman-alpha forest
Armengaud: Ultra-light scalar Dark Matter probed with the Lyman-alpha forest
16:30 - 16:55
I will introduce the main features of the so-called "fuzzy dark matter" (FDM) model, in which a (pseudo)scalar field with mass in the 10^{-24} - 10^{-20} eV range behaves as DE at high redshift, and DM at low z. I will review the growth of LSS in this scenario, in the linear as well as non-linear regimes. FDM is a good candidate to solve the so-called small-scale crisis of the CDM paradigm. I will then present constraints on FDM models derived from measurements of the small-scale Lyman-alpha forest flux power spectrum. Using a combination of SDSS-BOSS and higher-resolution spectra, we exclude FDM masses in the range 10^-22 - 3x10^-21 eV.
16:55
Moniez: Galactic Structure Measured from Microlensing
Moniez: Galactic Structure Measured from Microlensing
16:55 - 17:15
Tuesday, 26 September 2017
09:30
Kilbinger: Weak gravitational lensing peak counts as probe of dark energy and modified gravity
Kilbinger: Weak gravitational lensing peak counts as probe of dark energy and modified gravity
09:30 - 10:05
To include the full non-Gaussian information about cosmology and the large-scale structure from measurements of weak gravitational lensing, one needs to go beyond the second-order shear power spectrum. In my talk I will then focus on weak-lensing peak counts, an indirect probe of the halo mass function. I present a new fast and flexible model of peak counts. This model allows us to use new statistical inference methods that do not require assumptions about the functional form of the likelihood of the observables, e.g. Gaussianity. In particular, I will present results using Approximate Bayesian Computation (ABC), a new technique that has recently gained momentum in the astrophysics community. I will show some results and forecasts how peak counts can constrain dark energy and f(R) models.
10:05
Schmidt: Bias and modified gravity
Schmidt: Bias and modified gravity
10:05 - 10:40
Galaxy clustering is one of the key probes of large-scale structure, and hence of interest to tests of gravity as well. However, in order to make this probe robust, we need to understand the relation between the galaxy density and the underlying stress-energy and spacetime perturbations, i.e. bias. I will discuss the general bias expansion in the context of GR, and what changes in the case of frequently studied modified gravity scenarios.
10:40
Pujol: Mass mapping and galaxy bias in the Dark Energy Survey
Pujol: Mass mapping and galaxy bias in the Dark Energy Survey
10:40 - 11:05
The study of the large scale structures of the Universe is an important tool to learn about cosmology. The relation between the clustering of matter and the clustering of galaxies is known as galaxy bias. On the other hand, gravitational lensing allows us to measure the dark matter distribution from the shapes of the source galaxies. In this talk I will present the largest weak lensing mass maps to date obtained from the Dark Energy Survey Year 1 data which covers around 1500 square degrees. I will also present a method to measure tomographic galaxy bias in observations from the combination of galaxy density and weak lensing maps, developed in Pujol et al. 2016 and applied to the Dark Energy Survey in Chang et al. 2016.
11:05
coffee
coffee
11:05 - 11:30
11:30
Li: Cosmological tests of gravity - some recent updates
Li: Cosmological tests of gravity - some recent updates
11:30 - 12:05
Testing gravity on cosmological scales has received a great deal of interest in recent years in light of big galaxy surveys such as Eucild, LSST and DESI. In this talk I will describe some of the recent compelte and ongoing works in this development. The talk will begin with a description of the models begin studied and the rationales behind them, especially the generality of the results that would be derived from them. I will then talk about three main cosmological probes - weak gravitational lensing, galaxy clustering and clusters of galaxies - and their possible benefits and limitations in such tests.
12:05
Spurio Mancini: Testing Horndeski gravity with 3D weak lensing
Spurio Mancini: Testing Horndeski gravity with 3D weak lensing
12:05 - 12:25
We forecast the ability of future Euclid-like experiments to constrain Horndeski theories of gravity using a fully 3D cosmic shear analysis. We use the parametrization of the Horndeski Lagrangian density first proposed by Bellini&Sawicki(2014) based on four functions of time only, to constrain them by means of a Fisher matrix analysis. The constraints imply a fixed background cosmology, purely reflecting the change in structure growth, to which 3D weak lensing is particularly sensitive. This is due to the spherical Fourier-Bessel decomposition of the shear field that characterises the 3D formalism, which allows for inclusion and retention of the sources redshifts along the entire analysis. This has the advantage of following the evolution of structures in a non-averaged way, retaining more information on structure growth and how this is influenced by gravity.
12:25
Achitouv: "Probing dark energy with cosmic voids"
Achitouv: "Probing dark energy with cosmic voids"
12:25 - 12:50
Cosmic voids can supply powerful insights into the nature of dark energy, provided that we have accurate models of their statistical properties. In this talk I will present a new method to predict void density profiles, and show how we can reduce systematic errors when probing the growth rate around voids. This will be crucial for testing non-standard dark energy models with upcoming large survey campaigns. Finally, I will also present a self-consistent measurement of the growth rate around galaxies and around voids, in the 6- degree Field Galaxy Survey, as a test of the standard model of gravity.
12:50
Durrive: Constraining scalar field Dark Energy models
Durrive: Constraining scalar field Dark Energy models
12:50 - 13:15
13:15
lunch
lunch
13:15 - 14:45
14:45
Pierre: The cosmological analysis of X-ray cluster surveys
Pierre: The cosmological analysis of X-ray cluster surveys
14:45 - 15:10
We recall the bases of cosmological studies with clusters of galaxies. We present an original method that aims at determining the cosmological parameters, including the DE equation of state, by considering only the statistics of raw X-ray observables from a well defined cluster population. We illustrate the method with the XXL survey, which is the largest programme of XMM, the X-ray observatory of the European Space Agency.
15:10
Peel: Investigating a dark core: sparse reconstruction of the A520 cluster merger
Peel: Investigating a dark core: sparse reconstruction of the A520 cluster merger
15:10 - 15:35
15:35
Davis: Gravitational Waves in Doubly Coupled Bigravity
Davis: Gravitational Waves in Doubly Coupled Bigravity
15:35 - 16:10
In doubly coupled bigravity the two gravitons are coupled by a non-diagonal mass matrix and show birefringence. One of the two gravitons propagates with a speed which differs from one. This deviation is tightly constrained by both the gravitational Cerenkov effect and the energy loss of binary pulsars. When emitted from astrophysical sources, the wave form displays beats, which could be detected in future nano-Hertz interferometric experiments.
16:10
Lombriser: Challenges to Cosmic Self Acceleration in Modified Gravity from Gravitational Waves and Large-Scale Structure
Lombriser: Challenges to Cosmic Self Acceleration in Modified Gravity from Gravitational Waves and Large-Scale Structure
16:10 - 16:35
Scalar-tensor modifications of gravity have long been considered as an alternative explanation for the late-time accelerated expansion of our Universe. I will first show that a rigorous discrimination between acceleration from modified gravity and from a cosmological constant or dark energy is not possible with observations of the large-scale structure alone. I will then demonstrate how gravitational wave observations break this dark degeneracy and how the combination of the two challenges the concept of cosmic acceleration from a genuine scalar-tensor modification of gravity.
16:35
coffee
coffee
16:35 - 17:00
17:00
Blas: Using binary pulsars to test the dark sector
Blas: Using binary pulsars to test the dark sector
17:00 - 17:25
17:25
Zumalacarregui: Testing Dark Energy with Gravitational Waves
Zumalacarregui: Testing Dark Energy with Gravitational Waves
17:25 - 17:50
Scalar-tensor theories of gravity can provide viable models to explain cosmic acceleration and several discrepancies of standard cosmology such as the value of H0. I will present recent progress to understand these theories and determine the properties of gravity using gravitational waves and the large scale structure of the universe: The speed of gravitational waves will provide the most stringent test for a large class of theories, while a new generation of galaxy surveys will be sensitive to new relativistic effects on the largest cosmological scales. I will also introduce hi_class (www.hiclass-code.net), an accurate, fast and flexible code to compute cosmological predictions in a very large class of gravitational theories.
Wednesday, 27 September 2017
09:30
Bartolo: "Large Scale Structure in mimetic Horndeski gravity"
Bartolo: "Large Scale Structure in mimetic Horndeski gravity"
09:30 - 10:05
Within the so called mimetic gravity I will discuss cosmological perturbations for mimetic Horndeski models. I will focus on a proposal for a model of the dark universe, where both cold dark matter (CDM) and dark energy phenomena are described by a single component, the mimetic field. For the simpler minimal model it turns out that if the background expansion history is chosen to be identical to a perfect fluid dark energy (PFDE), then the mimetic model predicts the same power spectrum for the gravitational potentials as the PFDE. I will also discuss the distinguishability between these mimetic models and other popular models for DE. Finally I will present some preliminary results about the extraction of some parameters commonly used to quantify modifications w.r.t. to standard GR, like for example modifications of the Poisson equation.
10:05
Crisostomi: Higher Order Scalar-Tensor Theories
Crisostomi: Higher Order Scalar-Tensor Theories
10:05 - 10:30
Scalar-tensor theories of gravity play an essential role for building models of inflation and dark energy. For a very long time the focus has been placed on those theories leading to second order field equations, believing all the others plagued by instabilities. In this talk I will present new degenerate theories that, despite higher order in the equations of motion, are free from such a kind of pathology. Moreover, I will show that some higher order scalar-tensor theories are a useful tool to study parity violating effects in the gravity sector.
10:30
Saltas: "Challenging the consistency of scalar—field theories with derivative interactions from a fundamental viewpoint"
Saltas: "Challenging the consistency of scalar—field theories with derivative interactions from a fundamental viewpoint"
10:30 - 10:55
In this talk, I will discuss the consistency of a large class of theories for dark energy and primordial inflation from a fundamental point of view. In particular, focusing on the effective theory of a single scalar field exhibiting non—linear derivative interactions, I will discuss the ultraviolet properties of the theory at the 1—loop level and beyond, and argue about the significance of understanding the initial conditions and consistency of phenomenologically succesfull theories at sufficiently high energies.
10:55
coffee
coffee
10:55 - 11:30
11:30
Motohashi: "Healthy degenerate theories with arbitrary higher-order derivatives"
Motohashi: "Healthy degenerate theories with arbitrary higher-order derivatives"
11:30 - 11:55
Scalar-tensor theories serve models for inflation and dark energy. Many efforts have been made recently for constructing most general scalar-tensor theories with higher-order derivatives in their Lagrangian. Since higher-derivative theories are typically associated with Ostrogradsky ghost which causes unbounded Hamiltonian, it is important to clarify how to evade it. In this talk, I will discuss construction of healthy degenerate theories with higher-order derivatives which circumvent Ostrogradsky ghost. Generalizing the previous works on construction of ghost-free theories with second-order derivatives in Lagrangian, we clarify how to construct healthy theories with arbitrary higher-order derivatives. The necessary and sufficient condition for the absence of ghost degrees of freedom for theories with second-order derivatives is to eliminate linear dependence of canonical momenta in Hamiltonian. We find that this condition is not sufficient for theories with higher-than-second-order derivatives, and that linear dependence of canonical variables are also needed to be removed appropriately. We provide specific examples of healthy higher-order theories as well as ghost-free conditions for general theories with arbitrary higher-order derivatives to remove all the ghost degrees of freedom, under which we show that the Euler-Lagrange equations are reducible to a second-order system.
11:55
Vikman: Canonical Exorcism for Cosmological Ghosts
Vikman: Canonical Exorcism for Cosmological Ghosts
11:55 - 12:30
12:30
Barreira: "Galileon gravity: self-acceleration consistent with current cosmological data"
Barreira: "Galileon gravity: self-acceleration consistent with current cosmological data"
12:30 - 12:55
12:55
lunch
lunch
12:55 - 14:20
Thursday, 28 September 2017
09:30
Saridakis: "Torsional Modified Gravity and Cosmology"
Saridakis: "Torsional Modified Gravity and Cosmology"
09:30 - 10:05
Torsion has been proved to be crucial in gauging gravity, which is in turn a necessary step towards its quantization. On the other hand, almost all the efforts in modifying gravity has been performed in the usual curvature-based framework. We investigate theories of modified gravity based on its torsional-teleparallel formulation, and their cosmological applications. Moreover, we analyze the perturbations of the theory examining the growth history, we construct a cosmological bounce, and we use solar system and cosmological observations in order to impose constraints on the torsional modifications. Finally, we study the case where torsion is nonminimally coupled to a scalar field or its derivatives, as well as other extensions of the theory, using higher-order torsion invariants, or various torsion-matter couplings.
10:05
Heisenberg: “Vector-Tensor Theories”
Heisenberg: “Vector-Tensor Theories”
10:05 - 10:40
10:40
Pilo: "Cosmology of self-gravitating media"
Pilo: "Cosmology of self-gravitating media"
10:40 - 11:15
The low-energy dynamics of a generic self-gravitating media can be studied by using effective field theory in terms four derivatively coupled scalar fields. Imposing SO(3) internal spatial invariance, the theory describes fluids, superfluids, solid and supersolids. Dynamical and thermodynamical properties of the medium are dictated by internal symmetries of the effective theory. In the unitary gauge, where the scalar fields' fluctuations are gauged away, the most general medium can be equivalently described as rotational invariant massive gravity. From the analysis of cosmological perturbations it emerges that in the scalar sector, besides the gravitational potential, a non-adiabatic mode corresponding to the perturbations of entropy per particle σ is present. Perfect fluids and solids are adiabatic with constant in time σ while for superfluids and supersolids σ has non-trivial dynamics. Tensor perturbations are massive for solid and supersolid. Such an effective approach can be used to give a very general modelling of the dark sector based on symmetries.
11:15
coffee
coffee
11:15 - 11:45
11:45
Nunes: Dark energy couplings
Nunes: Dark energy couplings
11:45 - 12:20
12:20
Van de Bruck: "Interactions in the dark sector: the cosmology of conformally and disformally coupled dark matter"
Van de Bruck: "Interactions in the dark sector: the cosmology of conformally and disformally coupled dark matter"
12:20 - 12:55
A fifth force between the standard model particles is highly constrained. On the other hand, dark matter particles could interact for example via a force mediated by dark energy scalar field. Such interactions are currently constrained only by cosmological observations. In this talk I will discuss scalar-tensor theories of interacting dark matter-dark energy, allowing for both conformal and disformal couplings. I will discuss that while conformally coupled dark matter is strongly constrained by observations of CMB anisotropies and large scale structures, this is not the case for disformally coupled dark matter or mixtures between conformal and disformal couplings. After discussing the cosmological consequences of a disformal coupling term, I will present the latest constraints on both conformal and disformal couplings coming from diverse cosmological probes.
12:55
Nunes: "The cosmology of the de Sitter Horndeski models"
Nunes: "The cosmology of the de Sitter Horndeski models"
12:55 - 13:15
13:15
lunch
lunch
13:15 - 14:45
14:45
Deffayet: "Partially Massless Graviton on Beyond Einstein Spacetimes"
Deffayet: "Partially Massless Graviton on Beyond Einstein Spacetimes"
14:45 - 15:20
We show that a partially massless graviton can propagate on a large set of spacetimes which are not Einstein spacetimes. Starting from a recently constructed theory for a massive graviton that propagates the correct number of degrees of freedom on an arbitrary spacetime, we first give the full explicit form of the scalar constraint responsible for the absence of a sixth degree of freedom. We then spell out generic conditions for the constraint to be identically satisfied, so that there is a scalar gauge symmetry which makes the graviton partially massless. These simplify if one assumes that spacetime is Ricci symmetric. Under this assumption, we find explicit non-Einstein spacetimes (some, but not all, with vanishing Bach tensors) allowing for the propagation of a partially massless graviton. These include in particular the Einstein static Universe.
15:20
Burrage: The effect of screening on galactic dynamics
Burrage: The effect of screening on galactic dynamics
15:20 - 15:55
15:55
Wong: "Contemplating Atoms: What hydrogen teaches us about modified gravity"
Wong: "Contemplating Atoms: What hydrogen teaches us about modified gravity"
15:55 - 16:15
Considering simple systems can often be helpful in elucidating the most important features of a theory. I provide a recent example by revisiting the behaviour of hydrogen atoms in chameleon-like modified gravity, highlighting some recent advancements in our understanding. A careful analysis uncovers additional interaction terms in the Hamiltonian previously unaccounted for, which can dominate the chameleon-induced fine-structure corrections of certain spectral lines. Effects on hyperfine structure and on violations of the Einstein equivalence principle are also presented for the first time. While these developments enable modest updates to chameleon constraints based on atomic precision tests, they remain largely uncompetitive with other experimental bounds. Of greater value are the general insights gained from this study, and their possible implications for future work will be discussed.
16:15
coffee
coffee
16:15 - 16:45
16:45
Kading: "Chameleon-induced decoherence in an atom interferometer"
Kading: "Chameleon-induced decoherence in an atom interferometer"
16:45 - 17:10
Many modified gravity theories lead to the introduction of a new scalar field which would be expected to cause an additional gravity-like force. However, so far no solar system based observation could confirm the existence of such a fifth force. A way of explaining a force’s apparent absence is by a screening mechanism. For example, chameleon scalar fields obey to a mechanism by which they adapt their mass to the mass density of their environment. In this way, a force caused by chameleons is screened in our solar system due to the large effective mass of its carrier. Nevertheless, there are possible manners of observing chameleons even in earth based experiments. One way would be to look at the effect of the chameleon force on the decoherence of two parts of a wave function in an atom interferometer. I will present the method of calculating the time of chameleon-induced decoherence in such an experiment and current results of this calculation.
17:10
Ip: "Solar System Constraints on Disformal Gravity Theories"
Ip: "Solar System Constraints on Disformal Gravity Theories"
17:10 - 17:30
[Coauthors: Jeremy Sakstein, Fabian Schmidt] (arXiV: 1507.00568) We wanted to see if (Horndeskian) disformal theories of gravity can be a driving mechanism of cosmic acceleration. Local test constraints on PPN parameters encoding preferred-frame effects (due to the SS moving against the cosmological background) require these theories to have a cosmology indistinguishable from LCDM, under the assumption of the equivalence principle.
17:30
Nishimichi: "Response function and reconstruction for accurate tests of dark energy using clustering statistics on BAO scale"
Nishimichi: "Response function and reconstruction for accurate tests of dark energy using clustering statistics on BAO scale"
17:30 - 17:55
Friday, 29 September 2017
09:30
Liguori: "Constraining K-mouflage models with CMB data"
Liguori: "Constraining K-mouflage models with CMB data"
09:30 - 10:05
I will discuss the implementation of K-mouflage models of Modified Gravity in the EFTCAMB solver and its application to constraining K-mouflage theories using Planck data. I will show that, since K-mouflage presents a non-trivial expansion history at high-redshift, interesting bounds on relevant parameters can already be placed by looking at primordial CMB spectra. Finally, I will briefly discuss CMB-galaxy cross-correlation in K-mouflage scenarios, showing that also in this case an interesting phenomenology arises, due to the evolution of the growth factor in the matter dominated regime.
10:05
Fasiello: LSS probes of late-time cosmic acceleration
Fasiello: LSS probes of late-time cosmic acceleration
10:05 - 10:30
After a brief introduction on perturbative large scale structure probes of dark energy/modified gravity, I will describe a newly proposed phenomenological framework to account for screening mechanisms at mildly-non-linear scales.
10:30
coffee
coffee
10:30 - 11:00
11:00
Dhawan: "Narrowing down the possible explanations of cosmic acceleration with geometric probes"
Dhawan: "Narrowing down the possible explanations of cosmic acceleration with geometric probes"
11:00 - 11:35
Recent re-calibration of the Type Ia supernova (SNe~Ia) magnitude-redshift relation combined with cosmic microwave background (CMB) and baryon acoustic oscillation (BAO) data have provided excellent constraints on the standard cosmological model. Here, we examine particular classes of alternative cosmologies, motivated by various physical mechanisms, e.g. scalar fields, modified gravity and phase transitions to test their consistency with observations of SNe~Ia and the ratio of the angular diameter distances from the CMB and BAO. Using a model selection criterion for a relative comparison of the models (the Bayes Factor), we find moderate to strong evidence that the data prefer flat Λ CDM over models invoking a thawing behaviour of the quintessence scalar field. However, some exotic models like the growing neutrino mass cosmology and vacuum metamorphosis still present acceptable evidence values. The bimetric gravity model with only the linear interaction term can be ruled out by the combination of SNe~Ia and CMB/BAO datasets whereas the model with linear and quadratic interaction terms has a comparable evidence value to standard Λ CDM. Thawing models are found to have significantly poorer evidence compared to flat Λ CDM cosmology under the assumption that the CMB compressed likelihood provides an adequate description for these non-standard cosmologies. We also present estimates for constraints from future data and find that geometric probes from oncoming surveys can put severe limits on non-standard cosmological models.
11:35
Karmakar: "Cosmic structures in ghost-free scalar-tensor theories of gravity"
Karmakar: "Cosmic structures in ghost-free scalar-tensor theories of gravity"
11:35 - 12:00
In this article, we study the cosmic structures in the quadratic Degenerate Higher Order Scalar Tensor (qDHOST) model, which has been recently proposed as the most general scalar tensor theory without ghosts (up to quadratic dependence on the covariant derivatives of the scalar field). We explicitly provide the covariant field equations of general Higher Order Scalar Tensor (qHOST) and qDHOST. We then study a static, spherically symmetric object embedded in de Sitter space-time for the qDHOST model. This model exhibits breaking of the Vainshtein mechanism inside matter and Schwarzschild-de Sitter space-time outside the matter, where GR can be recovered. (To appear on arxiv soon.)
12:00
Marinoni: "E pur si muove! A real-time detection of our acceleration through space"
Marinoni: "E pur si muove! A real-time detection of our acceleration through space"
12:00 - 12:35
High-precision astrometric experiments will allow to detect our proper acceleration through space via real-time observations of the change in the aberration of sources at cosmic distances. This `Aberration Drift’ effect is a powerful consistency test of FLRW metric, it may set independent constraints on the amplitude of the Hubble constant and the linear growth rate of cosmic structures, and it may also be instrumental in searching for evidences of new physics beyond the standard model. I will present the formalism of this novel test of cosmology, discuss the physics to which it is sensitive and show simulated forecasts of the accuracy with which it can be implemented by ongoing satellite missions such as Gaia or upgraded future experiments.
12:35
lunch
lunch
12:35 - 14:00
14:00
Sawicki: Vorticity in the time of galaxy surveys
Sawicki: Vorticity in the time of galaxy surveys
14:00 - 14:35
Vorticity in the time of galaxy surveys
14:35
Lehebel: "The hair of compact objects in Horndeski theory"
Lehebel: "The hair of compact objects in Horndeski theory"
14:35 - 15:00
Compact astrophysical objects, like black holes and neutron stars, are going to open a new and enlightening window on gravity in the forthcoming years. The study of such objects in strong curvature regimes will a priori allow to test alternative gravity theories, like scalar-tensor models. I will discuss spherically symmetric and static objects in the framework of Horndeski theory, proving the absence of scalar hair for most models. I will also carefully classify the possible ways to escape this no-hair theorem.
15:00
Llinares: "Weighted density fields as improved probes of modified gravity models"
Llinares: "Weighted density fields as improved probes of modified gravity models"
15:00 - 15:25
15:25
Lewandowski: "EFT of Large-Scale Structure and EFT of Dark Energy"
Lewandowski: "EFT of Large-Scale Structure and EFT of Dark Energy"
15:25 - 15:50
In the next few years, large-scale structure (LSS) surveys will probe the low-redshift universe with unprecedented accuracy. Because there are more modes available at smaller scales, the amount of information about the the universe that we can extract from these surveys depends on our ability to theoretically understand these small, non-linear scales. Among other things, we hope to learn about the early universe (primordial non-Gaussianities) and the late universe (dark energy). The effective field theory of large-scale structure (EFTofLSS) is a theoretical framework that has allowed us to make accurate predictions in the mildly non-linear regime. In this talk, I will briefly review recent progress in the EFTofLSS and explore how it can be used to constrain interactions in the effective field theory of dark energy.
15:50
coffee
coffee
15:50 - 16:20
16:20
Ilic: "Cosmology of the Galileon extension of the TeVeS theory"
Ilic: "Cosmology of the Galileon extension of the TeVeS theory"
16:20 - 16:45
For more than a decade, many attempts have been made at developing a fully relativistic theory with Milgrom's MOND-like phenomenology. Many of these theories have a similar ambiguity in that all possess a function in the Lagrangian that must be chosen by hand. Babichev et al. (2011) proposed a model that avoids the use of such an unspecified function : this theory uses Bekenstein’s TeVeS theory as basis but extends it with the addition of a Galileon-type term (generating a convenient Vainshtein screening in high-curvature environment such as the solar system) and the removal of the free function. However, the viability of the theory in a cosmological context has yet to be proven. In this talk, I will present the results of a recent work where we tested this theory both at the level of the cosmological background evolution as well as the perturbed sector, using constraints from the latest cosmological microwave background observations.
16:45
de Fromont: "Testing modified gravity with cosmic voids and compensated structures"
de Fromont: "Testing modified gravity with cosmic voids and compensated structures"
16:45 - 17:10
These last years, cosmic voids have been used as original probes for gravity and dark energy. This is motivated by the fact that these regions are expected to be safe from both baryonic and non linear physics unlike galaxy clusters or DM halos. However, these approaches are limited by the absence of a fully consistent model for cosmic voids. In this talk, I will introduce a new model that provides predictions for both shape and statistics of these regions for any cosmology and redshift. Using this model, I will discuss their sensitivity to modified gravity such as f(R) theory and discuss the possibilities to constraint efficiently the nature of gravity in upcoming surveys.
Saturday, 30 September 2017
Sunday, 1 October 2017
Monday, 2 October 2017
11:00
Davis: Screening mechanisms in modified-gravity scenarios
Davis: Screening mechanisms in modified-gravity scenarios
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Winther: "COLA algorithm for faster simulations"
Winther: "COLA algorithm for faster simulations"
14:00 - 15:00
Tuesday, 3 October 2017
11:00
Charmousis: Compact objects in scalar-tensor and vector-tensor theories
Charmousis: Compact objects in scalar-tensor and vector-tensor theories
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Davis: Screening mechanisms in modified-gravity scenarios
Davis: Screening mechanisms in modified-gravity scenarios
14:00 - 15:00
15:30
Suroso: "Four Dimensional Cosmology with Nonminimal Derivative Coupling of External Scalar Field"
Suroso: "Four Dimensional Cosmology with Nonminimal Derivative Coupling of External Scalar Field"
15:30 - 16:00
The nonminimal derivative coupling (NMDC) model is a class of tensor scalar theory of gravity that contains a coupling between curvature tensor and derivative of scalar field. This model has been used in various aspects of gravity and cosmology including inflation, late time acceleration, and black hole physics. The dynamics of the model is described by the Einstein equations (which is obtained by varying the action with respect to the metric) and the scalar field equation of motion (which comes from the variation of the action with respect to the scalar field). In this talk, the scalar field is considered as an external scalar field, which means that we do not take a variation of the action with respect to the scalar field, and the field equations are derived from the Einstein equations and the conservation of energy momentum tensor. Then their solution is studied for some particular potential functions of scalar field.
Wednesday, 4 October 2017
11:00
Puchwein: "Numerical simulations of screened modified gravity models"
Puchwein: "Numerical simulations of screened modified gravity models"
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Charmousis / Babichev: Compact objects in scalar-tensor and vector-tensor theories
Charmousis / Babichev: Compact objects in scalar-tensor and vector-tensor theories
14:00 - 15:00
15:30
Sawicki + Vikman : "constraints on Horndeski theories"
Sawicki + Vikman : "constraints on Horndeski theories"
15:30 - 16:30
Thursday, 5 October 2017
11:00
Davis: Screening mechanisms in modified-gravity scenarios
Davis: Screening mechanisms in modified-gravity scenarios
11:00 - 12:00
12:30
lunch
lunch
12:30 - 14:00
14:00
Babichev: "Black holes in massive gravity"
Babichev: "Black holes in massive gravity"
14:00 - 15:00
15:00
Zumalacarregui: "scalar fields: local vs cosmological"
Zumalacarregui: "scalar fields: local vs cosmological"
15:00 - 16:00
16:00
Happy hour: beer, wine and biscuits
Happy hour: beer, wine and biscuits
16:00 - 17:00
Friday, 6 October 2017