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Home , CoRoT, Eddington (spacecraft), PROBA, Solar Orbiter, SWAP (instrument), Venus Express

EIRO School CERN May 2013

ESA Science Programme: Recent events & science results

David Lumb Research & Scientific Support Department , ESTEC

SCIENCE AND ROBOTIC EXPLORATION 1 EIRO School CERN May 2013

SCIENCE AND ROBOTIC EXPLORATION 2 EIRO School CERN May 2013

SCIENCE AND ROBOTIC EXPLORATION 3 Current ESA space science missions

Euclid JWST BepiColombo LISA Pathfinder PROBA-2 Herschel CoRoT Express Express INTEGRAL XMM-Newton Cassini- SOHO Hubble Implementation Operational

1990 1994 1998 2002 2006 2010 2014 2018 2022 4 EIRO School CERN May 2013 PROBA-2

ESA technology demonstrator / observatory, launched in November 2009

SCIENCE AND ROBOTIC EXPLORATION 5 EIRO School CERN May 2013 The approaching solar maximum

PROBA-2 SWAP daily 17.4nm images from 2 February 2010 to 26 October 2012

SCIENCE AND ROBOTIC EXPLORATION 6 EIRO School CERN May 2013 Total solar eclipse of November 13, 2012

SCIENCE AND ROBOTIC EXPLORATION 7 EIRO School CERN May 2013 Total solar eclipse of November 13, 2012

Centre: 17.4nm Fe IX (PROBA-2); middle: ground-based white- (Lecleire); outer: LASCO C2 (SOHO) / ESA, NASA, Koutchmy

SCIENCE AND ROBOTIC EXPLORATION 8 EIRO School CERN May 2013 SOHO

ESA-NASA solar observatory, launched 1995

SCIENCE AND ROBOTIC EXPLORATION 9 EIRO School CERN May 2013 Solar meridional flow Material transported from equator to poles Carries magnetic flux with it Poleward flow at ~15–20 m s–1 Operates in convective zone Related to 11 yr solar cycle Convective zone Flux carried to poles, builds up polar , then returns below surface

Hathaway & Rightmire Radiative ApJ, 2011 zone

Core Graphic: NASA MSFC Solar Physics

SCIENCE AND ROBOTIC EXPLORATION 10 EIRO School CERN May 2013 First detection of return flow Return flow not previously seen Must exist for conservation Slower due to higher density How slow & how deep? SOHO MDI Use supergranules as probe Cross-correlate MDI dopplergrams as function of intervening time delay Longer times correspond to larger cells, which extend deeper Equator-ward flow seen 4.6 ± 0.4 m s–1 at 70 Mm (10% R⊙) Important for dynamo models of Sun’s magnetic cycle

Hathaway 2012, ApJ

SCIENCE AND ROBOTIC EXPLORATION 11 EIRO School CERN May 2013 First detection of return flow Return flow not previously seen Must exist for mass conservation Slower due to higher density How slow & how deep? SOHO MDI helioseismology Use supergranules as probe Cross-correlate MDI dopplergrams as function of intervening time delay Longer times correspond to larger cells, which extend

deeper corresponding to depth of 70Mm Equator-ward flow seen 4.6 ± 0.4 m s–1 at 70 Mm (10% R⊙) Important for dynamo models of Sun’s magnetic cycle

Hathaway 2012, ApJ

SCIENCE AND ROBOTIC EXPLORATION 12 EIRO School CERN May 2013 Cluster

ESA magnetospheric physics mission, launched 2000

SCIENCE AND ROBOTIC EXPLORATION 13 EIRO School CERN May 2013 Turbulence at the reconnection scale Turbulence a ubiquitous phenomenon Thought to play key role in heating solar as it crosses interplanetary space cools as it expands, but much less than expected Simulation of decaying turbulence Perpendicular to interplanetary magnetic field and direction of solar wind flow Shows evolution of small-scale sheets between larger swirls in magnetofluid Cluster observations S/C separation ~ 20 km, 450 samples s–1 Revealed existence of current sheets and energy release at very small scales Heat dissipation due to reconnection? Solar Orbiter: true closer to Sun as well?

Simulations and Cluster data from Perri et al. 2012, PRL / ESA

SCIENCE AND ROBOTIC EXPLORATION 14 EIRO School CERN May 2013 Turbulence at the reconnection scale Turbulence a ubiquitous phenomenon Thought to play key role in heating solar wind as it crosses interplanetary space Solar wind cools as it expands, but much less than expected Simulation of decaying turbulence Perpendicular to interplanetary magnetic field and direction of solar wind flow Shows evolution of small-scale sheets between larger swirls in magnetofluid Cluster observations S/C separation ~ 20 km, 450 samples s–1 Revealed existence of current sheets and energy release at very small scales Heat dissipation due to reconnection? Solar Orbiter: true closer to Sun as well?

Simulations and Cluster data from Perri et al. 2012, PRL / ESA

SCIENCE AND ROBOTIC EXPLORATION 15 EIRO School CERN May 2013

ESA Venus planetary physics mission, launched 2005

SCIENCE AND ROBOTIC EXPLORATION 16 EIRO School CERN May 2013 A in the life of Venus Express

VEX VMC: see http://www.esa.int/Our_Activities/Space_Science/A_day_in_the_life_of_Venus_Express

SCIENCE AND ROBOTIC EXPLORATION 17 EIRO School CERN May 2013 When a looks like a comet

Magnetosphere and of Venus as induced by the solar wind Normal solar wind dynamic pressure: Trajectory of VEX in orbit around Venus Ionosphere confined close to planet on dayside on 4 Aug 2010 in cylindrical coords √ 2 2 Ionosphere truncated and chaotic on nightside (Rcyl = Y + Z , with X, Y, Z in Venus solar orbital coordinates)

Venus Express ASPERA + MAG / Wei et al. 2012, P&SS / ESA

SCIENCE AND ROBOTIC EXPLORATION 18 EIRO School CERN May 2013 When a planet looks like a comet

Magnetosphere and ionosphere of Venus as induced by the solar wind Normal solar wind dynamic pressure: Very low SWDP (4 Aug 2010): Ionosphere confined close to planet on dayside Ion channel opened to nightside “ ” Ionosphere truncated and chaotic on nightside Ionosphere extends into cometary tail

Venus Express ASPERA + MAG / Wei et al. 2012, P&SS / ESA

SCIENCE AND ROBOTIC EXPLORATION 19 EIRO School CERN May 2013

ESA Mars planetary physics mission, launched 2003

SCIENCE AND ROBOTIC EXPLORATION 20 EIRO School CERN May 2013 MEX HRSC approaching global coverage

Mosaic of 2072 HRSC swathes, covering 87.8% of planet (61.5% at < 20 m pix–1) by 30 June 2012

Mars Express HRSC, ESA / DLR / FU Berlin (G. Neukum), processed by Fred Jansen

SCIENCE AND ROBOTIC EXPLORATION 21 EIRO School CERN May 2013 Mars global mineralogy I

Near- (1.08 μm) albedo

Anhydrous nanophase ferric oxides (oxidised dusty materials)

MEX OMEGA 0.36–2.5 μm spectral mapping data, January 2004 – August 2010 / Ody et al. 2012, JGR / ESA

SCIENCE AND ROBOTIC EXPLORATION 22 EIRO School CERN May 2013 Mars global mineralogy II

Near-infrared (1.08 μm) albedo

Pyroxenes (rock-forming inosilicates, associated with igneous or metamorphic rocks)

MEX OMEGA / Ody et al. 2012, JGR / ESA

SCIENCE AND ROBOTIC EXPLORATION 23 EIRO School CERN May 2013 Mars global mineralogy III (in progress)

Olivines (Mg,Fe)2SiO4

High

grain grain size and/or high and/or abundance olivine high

Low High = high in relative relative content in high = High iron relatively and/or large

Olivines weather readily, so are relatively rare on surface of Mars Three different geological settings identified as olivine-bearing: Clusters of discontinuous patches on terraces around main basins: possibly related to excavated mantle ejectas Smooth inter-crater plains and smooth crater floors in southern highlands: possibly due to recent volcanic infilling Deposits in northern plains in dunes in crater floors, crater ejecta, exposed bedrock: primary olivine-rich basaltic units lie below sedimentary surface

MEX OMEGA / Ody et al. 2012, JGR, Ody et al. in preparation / ESA

SCIENCE AND ROBOTIC EXPLORATION 24 EIRO School CERN May 2013 Reull Vallis

MEX HRSC / ESA, DLR, FU Berlin (G. Neukum)

SCIENCE AND ROBOTIC EXPLORATION 25 EIRO School CERN May 2013 Reull Vallis perspective view

MEX HRSC / ESA, DLR, FU Berlin (G. Neukum)

SCIENCE AND ROBOTIC EXPLORATION 26 EIRO School CERN May 2013 Cassini-Huygens

NASA-ESA-ASI mission to the Saturnian system and Titan in particular, launched October 1997

SCIENCE AND ROBOTIC EXPLORATION 27 EIRO School CERN May 2013 A scale-model of the Nile on Titan

First example of extensive river system draining into a large sea Approximately 400 km long from headwaters to Ligeia Mare Likely filled with liquid methane-ethane: very low radar return

Cassini radar imaging data taken in September 2012 / NASA, ESA, ASI

SCIENCE AND ROBOTIC EXPLORATION 28 EIRO School CERN May 2013 ’ Titan s atmospheric reversal January 2010 September 2011 Reversal in global pole-to-pole circulation at the equinox Air above S pole began to cool and sink very soon after equinox; vortex appeared Enhancement of gases in high atmosphere due to photochemical reactions Vertical circulation results Thick atmosphere extends much higher than previously thought, up to ~ 600 km

Titan south , June 2012 / Cassini ISS

Cassini CIRS / Teanby et al. 2012, Nature / NASA, ESA, ASI

SCIENCE AND ROBOTIC EXPLORATION 29 EIRO School CERN May 2013 Hubble

NASA-ESA UV-optical-near-IR astrophysical observatory, launched 1990, last servicing May 2009

SCIENCE AND ROBOTIC EXPLORATION 30 EIRO School CERN May 2013 Hubble eXtremely Deep Field

10 years of ACS + WFC3 VIS data on HUDF field / Illingworth et al. 2012 / NASA, ESA

SCIENCE AND ROBOTIC EXPLORATION 31 EIRO School CERN May 2013 Hubble Ultra Deep Field 2012

Deeper WFC3 IR data on HUDF / Ellis et al. 2013, ApJL / NASA, ESA

SCIENCE AND ROBOTIC EXPLORATION 32 EIRO School CERN May 2013 Very high-z galaxy candidates

HUDF 2012 WFC3/IR, Ellis et al. 2013, ApJL / NASA, ESA

SCIENCE AND ROBOTIC EXPLORATION 33 EIRO School CERN May 2013 Hubble Frontier Fields

Abell 370 / HST ACS B,R,I / NASA, ESA, HST SM4 ERO team, ST-ECF

SCIENCE AND ROBOTIC EXPLORATION 34 EIRO School CERN May 2013 Hubble Frontier Fields

MACS J0416.1–2403

840 orbits of DDT time in 2013–2015 on six strong lensing galaxy clusters + parallel empty fields Cluster + parallel fields: ACS/WFC F435W, F606W, F814W to 3σ point source ~ AB 28.7–29.1 Cluster only: WFC3/IR F105W, F125W, F140W, F160W to 3σ point source ~ AB 28.6–29.0

’ Intrinsic science on galaxy evolution at high-z + broad legacy for JWST, ELT s, ALMA, VLA, etc.

Abell 370 / HST ACS B,R,I / NASA, ESA, HST SM4 ERO team, ST-ECF

SCIENCE AND ROBOTIC EXPLORATION 35 EIRO School CERN May 2013 Herschel Space Observatory

ESA-NASA far-infrared astrophysics observatory, launched 2009

SCIENCE AND ROBOTIC EXPLORATION 36 EIRO School CERN May 2013 W40: a cradle of

Herschel PACS + SPIRE, Gould Belt Survey, André et al. / ESA

SCIENCE AND ROBOTIC EXPLORATION 37 EIRO School CERN May 2013 Andromeda revisited

Herschel PACS + SPIRE consortia, O. Krause, HSC, H. Linz / ESA

SCIENCE AND ROBOTIC EXPLORATION 38 EIRO School CERN May 2013 formation across cosmic time Herschel-SPIRE galaxies (HSG) 1594 total at 250, 350, 500μm Lockman Hole N, GOODS-N, COSMOS, UDS, ELAIS-N1 fields Ancillary data available Spectroscopic follow-up Keck I LRIS, Keck II DEIMOS 767 with redshifts, 96% at z < 2 Peak redshift 0.85; max z ~5 Results HSG contribution to total SFR density significant from 0 < z < 2 IR-luminous galaxies (i.e. dusty starbursts) play important role in galaxy evolution, build-up of stellar mass over cosmic time

COSMOS field: Herschel SPIRE 250, 350, 500μm, survey, Oliver et al. / ESA

SCIENCE AND ROBOTIC EXPLORATION 39 EIRO School CERN May 2013 Star formation across cosmic time Herschel-SPIRE galaxies (HSG) 1594 total at 250, 350, 500μm Lockman Hole N, GOODS-N, COSMOS, UDS, ELAIS-N1 fields Ancillary data available Spectroscopic follow-up Keck I LRIS, Keck II DEIMOS 767 with redshifts, 96% at z < 2 Peak redshift 0.85; max z ~5 Results HSG contribution to total SFR density significant from 0 < z < 2 IR-luminous galaxies (i.e. dusty starbursts) play important role in galaxy evolution, build-up of stellar mass over cosmic time

COSMOS field: Herschel SPIRE 250, 350, 500μm, HerMES survey, Oliver et al. / ESA

SCIENCE AND ROBOTIC EXPLORATION 40 EIRO School CERN May 2013 XMM-Newton

ESA X-ray astrophysics observatory, launched 1999

SCIENCE AND ROBOTIC EXPLORATION 41 EIRO School CERN May 2013 An ultraluminous stellar-mass microquasar in M31

M31, Andromeda galaxy, XMM-Newton EPIC / Middleton et al. 2013, Nature / ESA

SCIENCE AND ROBOTIC EXPLORATION 42 EIRO School CERN May 2013 An ultraluminous stellar-mass microquasar in M31 XMMU J004243.6+412519 Detected on 15 Jan 2012 38 –1 Initially LX = 2 x 10 erg s Brightened by factor ~5 before fading Very bright, variable in radio Characteristics Initially hard power-law, cf. sub- accretion Later, similar to optically thick accretion disk at or above Eddington limit High-energy tail cf. Compton upscattering of disk in wind or photosphere Analysis Accreting stellar mass (~10M⊙) black hole with powerful jets Unobscured by galactic dust in plane ’ Thus, important template for low-L ULX s

M31, Andromeda galaxy, XMM-Newton EPIC / Middleton et al. 2013, Nature / ESA

SCIENCE AND ROBOTIC EXPLORATION 43 EIRO School CERN May 2013 INTEGRAL

ESA-Russia-NASA -ray astrophysics observatory, launched 2002

SCIENCE AND ROBOTIC EXPLORATION 44 EIRO School CERN May 2013 Tidal disruption of a planetary mass body NGC4845 NGC4845 / IGR J12580+0134 Detected by INTEGRAL on 2–10 Jan 2011 Follow-up XMM, MAXI, Swift observations Hard X-ray flux rose rapidly within few weeks, then declined over a year Characteristics DSS visible image Power-law , typical for accretion X-ray contours Time dependence of rise and fall indicative of tidal disruption event

Fast variations in X-ray flux near peak, giving black hole mass of ~ 3 x INTEGRAL hard X-ray flux 105 M⊙ Analysis Flare event consistent with tidal disruption of ~ 1–10MJup object, i.e. planetary mass body Predicted frequency ~ few 10–5 yr–1 galaxy–1 INTEGRAL could see a few decade–1 out to 50 Mpc

Combined INTEGRAL, XMM-Newton, MAXI, Swift data analysis, Nikołajuk & Walter 2012, A&A / ESA, NASA, JAXA

SCIENCE AND ROBOTIC EXPLORATION 45 EIRO School CERN May 2013 Planck

ESA cosmic microwave background experiment, launched 2009

SCIENCE AND ROBOTIC EXPLORATION 46 EIRO School CERN May 2013 Planck: first cosmology release! First all-sky image: July 2010 First data release: January 2011 Early Release Compact Source Catalogue Scientific papers on ERCSC, foregrounds Further science papers: January 2012 First cosmology: 21 March 2013 Press conference at ESA HQ, Paris Public release via Planck Legacy Archive All-sky CMB maps Component separations Derived data products Planck collaboration science papers In-depth science conference 47th ESLAB symposium, 2–5 April, ESTEC Cosmology and foreground science

SCIENCE AND ROBOTIC EXPLORATION 47 EIRO School CERN May 2013 Nearly a Standard Model ….. • For part, data agree extremely well with the 'standard model of cosmology' • Allow for a much improved measure of its parameters. • At the same time, the extraordinary quality reveals the presence of subtle anomalies in the CMB pattern • Most serious is a deficit in the signal at large angular scales on the sky, ~10% weaker than the standard model would like it to be. • Significant discrepancy of the CMB signal between two opposite hemispheres of the sky • Abnormally large 'cold spot' - are confirmed with high confidence. • Raises the possibility that the fabric of the cosmos, on the largest scales of the observable Universe, might be more

complex than we think. 48