… to millimetron instrument WG 12 m telescope Cooling: Y Single-dish & interferometry Wide freq range (FTS) Polarization mode Sensitivity:

Slides:

Advertisements

Similar presentations

Xavier Barcons Instituto de Física de Cantabria (CSIC-UC) On behalf of The Athena+ Co-ordination Group, the Athena+ Working Groups and Supporters A theme.

Advertisements

QUIET Q/U Imaging ExperimenT Osamu Tajima (KEK) QUIET collaboration 1.

The W i d e s p r e a d Influence of Supermassive Black Holes Christopher Onken Herzberg Institute of Astrophysics Christopher Onken Herzberg Institute.

End of Cosmic Dark Ages: Observational Probes of Reionization History Xiaohui Fan University of Arizona New Views Conference, Dec 12, 2005 Collaborators:

Dark Energy BAO Intensity Mapping T. Chang, UP, J. Peterson, P. McDonald PRL 100, (March 5, 2008) UP, L. Staveley-Smith, J. Peterson, T. Chang arXiv:

Low Energy measurements of Cosmic Rays suggested by the HE group 1 1Tracing the distribution of matter in order to understand HE data Measurements of NH.

On the nature of AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Leicester, March.

AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Accretion and ejection in AGN, Como,

Athena+, ESA’s next generation X-ray observatory Gregor Rauw High-Energy Astrophysics Group Liège University on behalf of the Athena+ coordination group.

The Science of JWST Caleb Wheeler. Table of Contents First Paper Second Paper Nervous standing after I finish early and everyone is too bored to formulate.

The Green Bank Telescope a powerful instrument for enhancing ALMA science Unblocked Aperture Low sidelobes gives high dynamic range Resistance to Interference.

The Transient Universe: AY 250 Spring 2007 Sagittarius A* Geoff Bower.

Towards the Grand Unification of AGNs in Hierarchical Cosmologies Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C.S. Frenk January 30,

Galaxies Types Dark Matter Active Galaxies Galaxy Clusters & Gravitational Lensing.

Galaxies with Active Nuclei Chapter 17. You can imagine galaxies rotating slowly and quietly making new stars as the eons pass, but the nuclei of some.

China’s Future Missions in Space High Energy Astrophysics Shuang Nan Zhang 张双南 Tsinghua University and Institute of High Energy Physics, Chinese Academy.

Moderator: Mitch Begelman Panelists: Stefi Baum Katherine Blundell Greg Madejski Paul Nulsen Łukasz Stawarz WHERE DO WE GO FROM HERE?

Quasar & Black Hole Science for GSMT Central question: Why do quasars evolve?

AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg.

Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)

Galaxy Formation Models Cold Dark Matter is the dominant component of galaxies and is key to their formation and evolution. CDM models have been wonderful.

X-ray Optical microwave Cosmology at KIPAC. The Survey 5000 square degrees (overlap with SPT and VISTA) Five-band (grizY) + VISTA (JHK) photometry to.

What Makes them Black Holes Other than the classical Rees argument about efficiency, size and luminosity what observational properties make these objects.

Quasars and Other Active Galaxies

Indian Astronomy Satellite Mission (ASTROSAT) National Institutions 1.ISRO, Bangalore 2.TIFR, Mumbai 3.IIA, Bangalore 4.RRI, Bangalore 5.PRL, Ahmedabad.

Black holes: do they exist?

P olarized R adiation I maging and S pectroscopy M ission Probing cosmic structures and radiation with the ultimate polarimetric spectro-imaging of the.

 Galaxies with extremely violent energy release in their nuclei  Active Galactic Nuclei (AGN)  Up to many thousand times more luminous than the entire.

Probing AGN physics with VLBI at Parkes Stas Shabala University of Tasmania.

1 BDRv3 - November 26, Markus Kissler-Patig E-ELT Programme 1 E-ELT Science Case Markus Kissler-Patig.

10 January 2006AAS EVLA Town Hall Meeting1 The EVLA: A North American Partnership The EVLA Project on the Web

BLACK HOLES: FROM STARS TO GALAXIES – ACROSS THE RANGE OF MASSES Felix Mirabel European Southern Observatory. Chile (on leave from CEA. France) In last.

Active Galaxies Definition – –Amount of Energy –Type of Energy Non-thermal Polarized Other characteristics –Emission spectra Hydrogen – Balmer series &

High energy Astrophysics Mat Page Mullard Space Science Lab, UCL 6. Jets and radio emission.

1 The XENIA mission The XENIA mission Cosmic chemical evolution of baryons Dieter H. Hartmann C. Kouveliotou, M. C. Weisskopf, J.W. den Herder, L. Piro,

AGN as extreme frontiers of our Universe H. Sol, LUTH, Observatoire de Paris ASTRONET meeting, Poitiers 2007.

Surveying the Universe with SNAP Tim McKay University of Michigan Department of Physics Seattle AAS Meeting: 1/03 For the SNAP collaboration.

RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing,

The Distributions of Baryons in the Universe and the Warm Hot Intergalactic Medium Baryonic budget at z=0 Overall thermal timeline of baryons from z=1000.

E-MERLIN : a pathfinder for the SKA (a summary of the e-MERLIN talk given at the Berkeley SKA meeting) e-MERLIN : a pathfinder for the SKA (a summary of.

Structure Formation in the Universe Concentrate on: the origin of structure in the Universe How do we make progress?How do we make progress? What are the.

Black holes and accretion flows Chris Done University of Durham.

Galaxies with Active Nuclei Chapter 14:. Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus).  “active galactic.

Observed and Simulated Foregrounds for Reionization Studies with the Murchison Widefield Array Nithyanandan Thyagarajan, Daniel Jacobs, Judd Bowman + MWA.

FIRST LIGHT A selection of future facilities relevant to the formation and evolution of galaxies Wavelength Sensitivity Spatial resolution.

KASI Galaxy Evolution Journal Club A Massive Protocluster of Galaxies at a Redshift of z ~ P. L. Capak et al. 2011, Nature, in press (arXive: )

The distant Universe and something about gravitational waves.

Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus). → “Active Galactic Nuclei” (= AGN) Up to many thousand.

Ay 191 Experiment Development of Hard X-ray Imaging Detectors J. Hong, B. Allen and J. Grindlay Hard X-rays (~5-600 keV) are direct probes of black holes:

Cosmology Lecture 10 The early universe. Our benchmark universe (  CDM) H 0 = 72 km s -1 Mpc -1  0 = 1 - spatially flat   = 0.73  m = 0.27  m,baryon.

The Submillimeter Array 1 David J. Wilner

10x Effective area JVLA, ALMA 10x Resolution w. 50% to few km + 50% to 300km Frequency range: 1 – 50, 70 – 115 GHz.

Science Drivers for Small Missions in High Energy Astrophysics Luigi PiroCAS-ESA Workshop – Chengdu Feb. 25, 2014 Science Drivers for Small Missions in.

Tidal Disruption Events

1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) Netherlands Institute for Radio Astronomy Astronomy at ASTRON George Heald.

Galaxy Evolution and WFMOS

Evidence from AGN for Binary Black Holes

Radio Loud and Radio Quiet AGN

Commissioning of ASTECAM

Galaxy Formation and Evolution: Where we are and where we are going.

Cherenkov Telescope Array

12/6/2018 Course Overview.

Observational Prospect of NIREBL

Dark Matter Limits From The Galactic Halo With H.E.S.S.

High Energy Astrophysics: problems and expectations

Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide.

Galaxies With Active Nuclei

Galaxies With Active Nuclei

Borislav Nedelchev et al. 2019

Presentation transcript:

… to millimetron instrument WG 12 m telescope Cooling: Y Single-dish & interferometry Wide freq range (FTS) Polarization mode Sensitivity: NEP \sim 10^{-19} ToO: 1hr-time scale repointing Camera size: 10^4 simultaneous pixels

Emission line galaxies (deep-field) cosmology: BAO + LSS blind search for SZE in clusters astrophysics: SFR, metallicity, UVB Global geometrical probes UCO + SLS pec.V + cosmological proper motion mod. G in extreme G environments (close to BH event horizon) probes of accretion flows and B-field effect & topology & feedback (BHs, microQSO, AGNs,QPO’s) accretion flows and warping effects (CO masers, AGNs, micro-QSOs) Acceleration mechanisms around BH and in jets (imaging and spectral evolution, polarization) double QSOs and X-shaped objects interferomety,. Spectra, polariz.) Search for WarmHoles and observational probes (B-field, intensity variations, interferometry, polariz.) Dwarf stars Rydberg atoms and B-field effects (single-dish, spectra, polariz.) Spectral and spatial microsctructure of CM; B fluctuations (molecules at high-z) (Dark Ages of the Universe) probing SMBH (primordial BHs) at z>10 SZE spectro-polarimetry and imaging clusters: cosmoogy, Dark Matter, dark Energy, mod-G,… RG lobes: evolution and acceleration processes B_field effect: polarization ToO: GRBs, SNRs, transients,.. (1hr re-pointing)