The science potential of atmospheric Cherenkov arrays used as - - PowerPoint PPT Presentation

The science potential of atmospheric Cherenkov arrays used as intensity interferometers

Willem-Jan de Wit w.j.m.dewit@leeds.ac.uk Michael Daniel for

H.E.S.S. VERITAS

Atmospheric Cherenkov Telescope Arrays

• Multiple telescopes image the source of optical Cherenkov light created by charged

secondary particles (“the shower”) from an incoming gamma-ray.

• The faint Cherenkov light requires large light collectors.
• The brief (~nanosecond) Cherenkov flash requires fast photon detectors.
• Shower image reconstruction gives spectral and angular information on the incoming

gamma-ray, hence many telescopes covering long baselines.

Similar technical specs of ACTs and I.I.

• Fast photon counters/digital

processing

• (very) Large photon collectors
• Large number of telescopes
• Telescope can point independently
• Long baselines

e.g. Le Bohec & Holder (2006) Bernloehr et al. (2007) red dots : 85m2 dish blue dots : 600 m2 dish

A proposed CTA lay-out ACT projects under study:

• CTA (EU)
• AGIS (US)

89 telescopes = 3916 baselines

What do stellar astronomers want? (apart from some fun) The accurate determination of the physical properties of stars, i.e. mass, radius, luminosity and elemental abundances ... and everything that either is ex- or accreted from/onto the star.

limiting magnitude

Sensitivity of CTA as an I.I.

(from Hanbury Brown 1973)

mv=8.5

S/ NRMS=A⋅⋅nph⋅

∣d∣

2⋅f⋅T /2

• S/N = 5
• A = 100 -- 600 m2
• quantum efficiency 30%
• n = 5.0 e-5 (1.0e-4)
• degree of coherence = 0.5
• bandwidth 1 GHz
• exposure time 5h

Le Bohec & Holder (2006) [mv= 9.25 using flux zeropoint of Bessel et al (1990)]

In a simple perspective ...

How many main sequence stars can be imaged (Mv<9.25)?

Three science case examples:

• Young stars
• Rapidly rotating stars
• Cepheids and distance scale

Science case: young stars

• the internal stellar structure of pre-main sequence stars
• chromospheric activity (cool spots)
• accretion activity (hot spots)

Palla & Stahler (2000) Nearby star formation regions:

• val: 50 pc

small blue dots: Beta Pic Ass. small red dots: Tucana/Horologium Ass. grey dot: Pleiades large blue dot: Beta Pic

50pc ~50 young stars with mv<8m In the last decade several young coeval stellar groups have been discovered in close proximity (~50pc) to the sun. Their closeness means the members are bright and renders the co-moving group relatively sparse – making them suitable, unconfused, targets even with the large optical PSF for an IACT (~few arcminutes).

• The spectral type range from A to G
• Sparse, therefore incomplete

membership (N(*) will increase!)

• Ages between 8-50Myr: a

substantial fraction still in the pre-main sequence contraction phase Zuckerman & Song (2004)

Science case: young stars

In the solar neighbourhood

Boden et al. 2005

The internal structure of young stars

and the calibration of pre-main sequence tracks ...

Interferometry of (non-eclipsing) spectroscopic binaries deliver dynamical masses (e.g. Boden et al. 2005), in combination with spectroscopic data.

• Components V mags: 6.9 and 8.0 at 45pc
• Based on 34 Keck-I interferometry

measurements In addition:

• Known distances (Hipparcos, GAIA

[launch 2011]) allow direct comparison of the predicted and I.I. observed sizes of individual PMS stars.

From PMS tracks masses are inferred. They are therefore fundamental for a correct understanding of the star formation process.

hot spots deliver direct information regarding the accretion of material onto the stellar surface cool spots (similar to sunspots) may cover 50% of the stellar surface and are the product of the slowly decaying rapid rotation of young stars

The surface structure of young stars

Magnetically guided accretion process (accretion funnel)

T Tauri

Understanding chromospheric activity and stellar magnetic fields

The surface structure of young stars

Doppler images of PW And Strassmeier & Rice (2006)

• 20Myr, K2V T Tauri star @ 40pc
• Magnitude in V-Band 8.7
• Cool spots are 1200K cooler than

stellar photosphere

• Cool spots may cover ~50% of surface
• > 65 stars have been doppler imaged

(Strassmeier 2002)

Understanding chromospheric activity and stellar magnetic fields

Inferred brightness distribution from Doppler imaging

The surface structure of young stars

• 2Myr, M0 T Tauri star @ 150pc
• Magnitude in V-Band 14
• Accretion spots are 2000K hotter

than stellar photosphere

Hot spots and the magnetic accretion phenomenon

Doppler imaging of MN Lupi

=>

The surface structure of young stars

• inferred morphology in

agreement with the magnetospheric accretion model

• the star's fast rotation (a factor
• f ~4 from break-up) suggests

that accretion could be responsible for spin-up, and hence strong activity

• magnetic field strength can be

inferred from comparison with models (Strassmeier et al. 2005)

Hot spots and the magnetic accretion phenomenon

Angular size estimate from I.I. and the Cepheid radius estimate from Baade-Wesselink method R1 R2 T1 T2 The radius of the cepheid can be determined from the observed radial velocities.

dR dT =v t

high resolution spectroscopy

Science case: distance scale

The zero-point of the Cepheid period-Luminosity relation

Baade-Wesselink method:

• 1. ∑(vspectro*∆t) = R2-R1
• 2. L1/L2 = R1/R2

D θ Angular size measurement (θ) from intensity interferometry Comparison of angular size and Baade-Wesselink determined size gives the distance to the Cepheid

Science case: distance scale

The sizes of Cepheids

Davis et al. 2008 using Sydney University Stellar interferometer (1 Cepheid) Lane et al. 2000/2002 with the Palomar testbed interferometer (2 Cepheids) Kervella et al. 2004 with the Very Large Telescope Interferometer (7 Cepheids)

~60 cepheid variables with mv<8m +

Classical Be stars are well-known for the presence of a circumstellar gaseous disk (the “e” in Be-type stars). The disk is formed in a mass-loss process from the star, and comes and goes (timescale of months to decades). It is bright in the NIR (Brehmsstrahlung).

Science case: rapidly rotating stars

Extremely distorted stars near (at?) break-up velocity

ζ Tauri in Hα at MkIII optical interferometer (2 telescopes)

Quirrenbach et al. (1994)

Townsend et al. 2004

• Be stars are extremely fast rotators
• How close to break-up?
• Insensitivity of line-width to

rotational velocity

• Pulsations probably also an important

ingredient

Classical Be disks : how to make them?

Science case: rapidly rotating stars

Von Zeipel effect/gravity darkening 0km/s 300km/s 400km/s 300km/s 487km/s

• wocki

spectral measurements of rotation can only provide lower limits

Domiciano de Souza et al. 2003

Science case: rapidly rotating stars

• VLTI-VINCI (K-band!, 2 telescopes)
• alpha Eridani: « Flattest star ever seen »
• v_rot (spectro) ~225 km/s
• v_rot (interfero) ~350 km/s (~break-up)

The measurement of a deformed star

• ~300 stars with mv<8m corresponding to a distance limit of 700pc
• 50% fraction of B0 stars showing Be phenomenon (i.e. an important

concept within stellar evolutionary theory)

• The disk formation and dissolution are poorly understood

Science case: rapidly rotating stars

Extremely distorted stars near (at?) break-up velocity

Simple examples: baseline coverage

Nbaseline = Ntel * (Ntel-1)/2. = 3916 (1060 independent baselines) 89 telescopes

Simple examples I : perfectly dark spot

Original Image Power spectrum Reconstructed image 3 milli arcsecond 1 single observation with a full 89 telescope CTA array, using phase information.

Original Image Power spectrum Reconstructed image 3 milli arcsecond

Simple examples II : Be star

1 single observation with a full 89 telescope CTA array, using phase information.

Simple examples III : T Tauri

Original Image Power spectrum Reconstructed image 3 milli arcsecond 1 single observation with a full 89 telescope CTA array, using phase information.

Science Summary

• Young stars:
• Internal stellar structure by means of dynamical masses of binaries
• PMS stellar radii in combination with known distances (GAIA)
• Stellar rotation, cool spots and dynamo action
• Hot spots and accretion phenomena (less certain)

At least 50 young stars for which CTA-I.I. could provide images

• Distance scale:
• Sizes of Cepheid variables to calibrate zeropoint of period-luminosity relation
• Rapidly rotating stars:
• Unambiguous determination of the rotational velocities of Be stars

Not or briefly discussed:

• X-ray binaries : 15 HMXB and 2 LMXB are brighter than 9.25 in V-band

(from the on-line X-ray binary catalogue (www.xrbc.org)

• Planetary transits (perfectly dark spot)

“Since astronomers study objects beyond their control, an imaging CTA-I.I. will provide a wealth of new discoveries”

Further reading The potential for intensity interferometry with γ-ray telescope arrays de Wit et al. arXiv:0710.0190 Towards μ-arcsecond spatial resolution with Air Cherenkov Telescope arrays as optical intensity interferometers de Wit et al. arXiv:0811.2377

fin?