The Search for Extraterrestrial Intelligence (SETI) Sir Bernard Lovell Chair, Prof. of Astrophysics. Director Jodrell Bank Centre for Astrophysics
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1 The Search for Extraterrestrial Intelligence (SETI) Mike Garrett e-merlin & SKA Sir Bernard Lovell Chair, Prof. of Astrophysics. Director Jodrell Bank Centre for Astrophysics Mike Garrett Sir Bernard Lovell Chair of Astrophysics, Director Jodrell Bank Centre for Astrophysics (JBCA).
2 e-merlin (SKA Pathfinder) operating at cm-λ with µjy sensitivity and ~ km baselines. e-merlin - introduction JBCA: telescopes we operate
3 e-merlin upgrade performance z=0.19 Javier Molden et al.
4 e-merlin e-merlin continues to be a very capable telescope addressing a broad range of different science cases.
5 Competitiveness Competitiveness - a unique radio facility: - microjy sensitivity at cm wavelengths with subarcsecond resolution across the full frequency range. Telescope upgrades being performed across the globe: ngvla (USA) LOFAR 2.0 (NL) GMRT upgrade (IN) FAST (CN) ASKAP (AU) MeerKAT (RSA) APERTIF (NL) MWA-256 (AU/USA) HERA (USA) LWA (USA) DSA (USA) CHIME (CA).. LSS (FR) MeerKAT ASKAP J-VLA
6 e-merlin Upgrade (2018) A proposal was recently submitted to STFC (PPRP) which aims to secure operational funding for the next 5 years ( ). A second proposal was submitted seeking funds for an upgrade of the telescope that would take it well into the SKA era.
7 e-merlin
8 Javier Molden et al.
9 Modular, non-disruptive Upgrade Plan New receivers, new frequency ranges: e-merlin S-band X-band e-merlin upgrade 1 GHz 10 GHz 25 GHz 100 GHz
10 Modular, non-disruptive Upgrade Plan New receivers, new frequency ranges: e-merlin S-band X-band e-merlin upgrade 1 GHz 10 GHz 25 GHz 100 GHz Broader bandwidths: 2 GHz => 8 GHz
11 Modular, non-disruptive Upgrade Plan New receivers, new frequency ranges: e-merlin S-band X-band e-merlin upgrade 1 GHz 10 GHz 25 GHz 100 GHz Broader bandwidths: Wider Field of View: 2 GHz => 8 GHz FoV ~ x9
12 New telescopes: Modular, non-disruptive Upgrade Plan SKA antenna at Defford increases sensitivity & improves uv-coverage at X- band + testbed for SKA AIP research. 1 GHz JBCA: telescopes we operate Defford Goonhilly
13 New telescopes: Modular, non-disruptive Upgrade Plan SKA antenna at Defford increases sensitivity & improves uv-coverage at X- band + testbed for SKA AIP research. 1 GHz JBCA: telescopes we operate Goonhilly doubles array resolution and improves uvcoverage for southern sources. Goonhilly Defford
14 New Capabilities: Modular, non-disruptive Upgrade Lovell + e-merlin telescopes beam-formed into a super-sensitive single aperture. 1 GHz Lovell
15 New Capabilities: Modular, non-disruptive Upgrade Lovell + e-merlin telescopes beam-formed into a super-sensitive single aperture. 1 GHz Lovell
16 Building on UK SKA Investment/Expertise JBCA: telescopes we operate
17 Building on UK SKA Investment/Expertise JBCA: telescopes we operate
18 Building on UK SKA Investment/Expertise Grainge et al. Jones et al. JBCA: telescopes we operate Alexander, Scaife et al. UK SKA Regional Science Node
19 Building on UK SKA Investment/Expertise Grainge et al. Jones et al. JBCA: telescopes we operate UK SKA Regional Science Node Alexander, Scaife et al. e-merlin will utilise SKA SDP software environment/infrastructure to improve throughput and science productivity.
20 Tes;ng General Rela;vity (Strong Regime, Gravita;onal Waves) Cosmic Dawn (First Stars and Galaxies) JBCA: telescopes we operate Cradle of Life (Planets, Molecules, SETI) Galaxy Evolu;on (Normal Galaxies z~2-3) Cosmic Magne;sm (Origin, Evolu;on) Cosmology (Dark Energy, Large Scale Structure) Explora;on of the Unknown Extremely broad range of science!
21 e-merlin vs SKA1-mid Collecting area of e-merlin (including Lovell Telescope) is ~ 1/3 collecting area of SKA-1 mid.
22 e-merlin vs SKA1-mid Collecting area of e-merlin (including Lovell Telescope) is ~ 1/3 collecting area of SKA-1 mid. e-merlin and SKA1-mid ~ similar frequency range.
23 e-merlin vs SKA1-mid Collecting area of e-merlin (including Lovell Telescope) is ~ 1/3 collecting area of SKA-1 mid. e-merlin and SKA1-mid ~ similar frequency range. e-merlin and SKA1-mid ~ similar baseline length.
24 e-merlin vs SKA1-mid Collecting area of e-merlin (including Lovell Telescope) is ~ 1/3 collecting area of SKA-1 mid. e-merlin and SKA1-mid ~ similar frequency range. e-merlin and SKA1-mid ~ similar baseline length. SKA uv-coverage is >> e-merlin
25 e-merlin vs SKA1-mid Collecting area of e-merlin (including Lovell Telescope) is ~ 1/3 collecting area of SKA-1 mid. e-merlin and SKA1-mid ~ similar frequency range. e-merlin and SKA1-mid ~ similar baseline length. SKA uv-coverage is >> e-merlin Shared software environment with Small-N, large-d presenting some processing advantages
26 Science Case Pulsars, Gravity & Gravitational Waves Time domain and Transient astrophysics Planet & Star formation Galaxy formation & evolution Weak & Strong Gravitational Lensing Addressing multiple STFC key challenges, incl. a broad range of astrophysics/cosmology/fundamental physics.
27 Science Case Pulsars, Gravity & Gravitational Waves Time domain and Transient astrophysics Planet & Star formation Galaxy formation & evolution Weak & Strong Gravitational Lensing Addressing multiple STFC key challenges, incl. a broad range of astrophysics/cosmology/fundamental physics.
28 Pulsars, Gravity & Gravitational Waves Combined e-merlin/lovell telescope fantastic Pulsar facility Gravitational waves & testing Gravity in Extremes: Lovell Telescope participates in EPTA & LEAP (Stappers et al.) - Galactic scale GW detector! New window on the Universe - nhz GWs = supermassive BH mergers - mass assembly in the early universe - stochastic (anisotropic) background LT+e-MERLIN - major addition to LEAP. STFC challenges: C1, C2, C6, D1, D2, D3
29 Pulsars, Gravity & Gravitational Waves Combined e-merlin/lovell telescope fantastic Pulsar facility Gravitational waves & testing Gravity in Extremes: Lovell Telescope participates in EPTA & LEAP (Stappers et al.) - Galactic scale GW detector! New window on the Universe - nhz GWs = supermassive BH mergers - mass assembly in the early universe - stochastic (anisotropic) background LT+e-MERLIN - major addition to LEAP. Radio follow-up of electro-magnetic counterparts to gravitational wave events STFC challenges: C1, C2, C6, D1, D2, D3
30 Science Case Pulsars, Gravity & Gravitational Waves Time domain and Transient astrophysics Planet & Star formation Galaxy formation & evolution Weak & Strong Gravitational Lensing Addressing multiple STFC key challenges, incl. a broad range of astrophysics/cosmology/fundamental physics.
31 Time domain and Transient astrophysics Fast transients e.g. Fast Radio Bursts (FRBs). FRBS: exotic phenomena associated with extremes of gravity, magnetism and energy (Lorimer et al. 2007). - huge event rate ~ 5-10,000 per day - almost certainly extragalactic (Chaterjee et al. Tendulkar et al. Marcotte et al. 2017) Marcotte et al Bassa et al STFC challenges: A6, D1, D2, D3
32 Time domain and Transient astrophysics Fast transients e.g. Fast Radio Bursts (FRBs). FRBS: exotic phenomena associated with extremes of gravity, magnetism and energy (Lorimer et al. 2007). - huge event rate ~ 5-10,000 per day - almost certainly extragalactic (Chaterjee et al. Tendulkar et al. Marcotte et al. 2017) Marcotte et al FRBs can be very interesting probes of cosmology - their dispersion measure also permits us to track the ionisation history of the universe as a function of cosmic time. We need to find more! Commensal LOFT-e (Localisation of Fast Transients with e-merlin - Stappers et al.) will piggy-back on e- MERLIN observations, waiting for FRB events and then localise them. Bassa et al STFC challenges: A6, D1, D2, D3
33 Science Case Pulsars, Gravity & Gravitational Waves Time domain and Transient astrophysics Planet & Star formation Galaxy formation & evolution Weak & Strong Gravitational Lensing Addressing multiple STFC key challenges, incl. a broad range of astrophysics/cosmology/fundamental physics.
34 Proto-planetary Simulations Scaled HL Tau model with pebble concentrations z=0.19 Javier Molden et al.
35 Science Case Pulsars, Gravity & Gravitational Waves Time domain and Transient astrophysics Planet & Star formation Galaxy formation & evolution Weak & Strong Gravitational Lensing Addressing multiple STFC key challenges, incl. a broad range of astrophysics/cosmology/fundamental physics.
36 The local universe Galaxy formation & evolution e-merlin - seeing through the dust in M82+ + with exquisite resolution (D~4Mpc): - decomposing galaxies into 100s of SF regions, SNR/SNe, UC HII regions. - Galactic-style physics of SF (and accretion) related phenomena on sub-pc scales. Moving out to 120 Mpc merging LIRG NGC6670 HST WFPC3/e-MERLIN (Alberdi et al. & LIRGI/GOALS team). Beswick et al. STFC challenges: A5, A6, D1, D3
37 Galaxy formation & evolution The distant universe e-merlin deep fields e-merge - e-merlin legacy project - Muxlow et al. - unique unobscured window on the co-evolution of accretion and star formation processes from z~ only e-merlin s resolution and sensitivity can decompose SF/AGN components - VLA observations at 10 GHz miss steep-spectrum SF emission ~5kpc e-merlin M dust obscured irregular galaxy Peak 24µJy/bm z=0.422 CI 6.75µJy/bm VLA resolution at 1.5GHz VLA 10GHz E. Murphy STFC challenges: A5, A6, D1, D3
38 Science Case Pulsars, Gravity & Gravitational Waves Time domain and Transient astrophysics Planet & Star formation Galaxy formation & evolution Weak & Strong Gravitational Lensing Addressing multiple STFC key challenges, incl. a broad range of astrophysics/cosmology/fundamental physics.
39 Cosmic shear & Gravitational Lensing e-merlin - pioneer of weak & strong lensing SuperCLASS - attempt to detect weak lensing signal in the radio (Brown et al.). RMS noise 1deg 2 - exploiting e-merlins sensitivity and resolution, and polarisation capabilities. - several Abell clusters in the field. - complimentary to optical weak lensing. STFC challenges: A5, A6, D1, D3
40 Cosmic shear & Gravitational Lensing e-merlin - pioneer of weak & strong lensing SuperCLASS - attempt to detect weak lensing signal in the radio (Brown et al.). RMS noise 1deg 2 - exploiting e-merlins sensitivity and resolution, and polarisation capabilities. - several Abell clusters in the field. - complimentary to optical weak lensing. Strong lensing (McKean, Jackson et al.). - EVN+e-MERLIN imaging of lenses testing DM models (CDM, WDM) - Searching for substructure in lens galaxy through image/lens model analysis in the uvplane - substructure that is not predicted by the model is evidence for DM e.g. massive black holes. - using lenses as natural telescopes (magnification). STFC challenges: A5, A6, D1, D3
41 Jodrell Bank Centre for Astrophysics Jodrell Bank Discovery Centre
42 Jodrell Bank Centre for Astrophysics Jodrell Bank Discovery Centre
43 Summary A SKA pathfinder telescope! - 30% of the collecting area of SKA1-mid - New receivers with broad frequency range: 1-25 GHz - Instantaneous bandwidth of up to 8 GHz - Good imaging capability (incl. equatorial fields) - MicroJy sensitivity with superb sub-arcsecond angular resolution - Accessible to full community - excellent user support - a factor of 10x better FoV at lowest frequencies
44 Summary A SKA pathfinder telescope! - 30% of the collecting area of SKA1-mid - New receivers with broad frequency range: 1-25 GHz - Instantaneous bandwidth of up to 8 GHz - Good imaging capability (incl. equatorial fields) - MicroJy sensitivity with superb sub-arcsecond angular resolution - Accessible to full community - excellent user support - a factor of 10x better FoV at lowest frequencies An upgraded e-merlin will prepare, train and grow the SKA science & engineering community, ensuring UK leadership in key areas in the run up to SKA1-mid operations.
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