mini-workshop
Fundamental Physics
ESO/Garching
18-19 Sep, 2014
С.А. Левшаков
Физико-технический институт им. А.Ф. Иоффе
Санкт-Петербург
E-ELT
adaptive, automatically correcting the atmospheric disturbances
six sodium (Na) laser guide stars
greater details than the HST by 15 times (!)
THE SCHEDULE OF THE E-ELT
Dome acceptance — March 2017Main structure acceptance — March 2020Technical first light — December 2021Instruments 1 and 2 first light — June 2022Start of observatory operations — October 2022.
OPEN QUESTIONS FOR THE E-ELT
1. EXOPLANETS: first direct images of Earth-like planets
2. FUNDAMENTAL PHYSICS: were the physical constants indeed constant over the history of the Universe?
3. BLACK HOLES:studies of the black hole at the center of the MW to reveal the nature of this object
4. STARS:when did the first stars form?
5. GALAXIES : individual stars in galaxies out to distances of ~ 10 Mpc
6. THE DARK AGES: can we observe the earliest epoch of the Universe?
Ryan Cooke (UCSC)Primordial deuterium in the era of the E-ELT
Velocity Relative to z = 3.0672594 (km/s)
Direct evidence for new physics ...
consistency tests
can only be trusted
once
it is seen through independent probes
Tz /T
0 ~ (1+z)(α
z /α
0 )1/4
~ (1+z)(1 + Δα14 α )
but standard cosmology assumes adiabatic expansion and photon number conservation
a robust prediction of standard cosmology
T(z) = T0 (1+z)
violated in many scenarios, including string theory etc.
T(z) = T0 (1+z)1-β
Constraints on TCMB
(z) using UV absorption linesPasquier Noterdaeme (IAP)
C II* E01
= 63.4 cm-1
C I* E02
= 43.4 cm-1
C I* E01
= 16.4 cm-1
CO E01
~ kTCMB
CO excitation diagram based on T01
, T02
, and T12
long dashed line – expected TCMB
= 9.315 ± 0.007 K
at z = 2.4185 from the hot BB theory
Michael Murphy (Swinburne University of Technology)
The future of varying α searches at ESO
Long-range distortions!
Sebastien Muller (Onsala Space Observatory)
The z = 0.89 molecular absorber toward the lensed
blazar PKS 1830-211
continuum map at 3 mm HST
S. A. Levshakov
Local tests of spatial variation of me/m
p
Effelsberg 100-m telescope
line width ~ 0.2 km/s
~ 0.001 km/s
~ 0.005 km/s
line position uncertainty
Δμ/μ < 2 10-8 (3σ)
How to improve current Δμ/μ estimates ?
JK
=11- 2
1644.4 GHz, i.e. in B9 ALMA band1215.2
GHz
rotational transition of para-NH3
z = 0.89
para- vs ortho-NH3
!
Persson et al. 2010
Different absorption patterns !
Herschel/HIFI observations of para- and ortho-NH3 rotational transitions
VLSR
robust approach – to use para-NH3 only
Extragalactic NH3 absorption detected
HFLS3dusty star-forming galaxy (DSFG) z = 6.34Riechers et al. 2013
if z > 1then ground-based telescopes can be used to observe 1.2 THz line
for σV ~ 0.1 km/s, S/N ~ 30, and ΔV ~ 20 km/s (like PKS1830-211)
Δμ/μ ~ 10-7 (based on NH3 only)
Hydronium H3O+
frequencies are in GHz
11-2
1 307 GHz
32-2
2 364 GHz
30-2
0 396 GHz o-H
3O+
p-H3O+
p-H3O+
Q
-3.0
-3.5
+6.4
Kozlov & Levshakov 2011Kozlov, Porsev, Reimers 2011
p-H3O+ : ΔQ = Q
307 – Q
364 = 9.9
3 times ΔQammonia
(for ALMA)
H3O+ observations (star-forming regions, MW)
CSO 10.4-m telescope (Phillips et al. 1992)
also detected towards
Orion-KL, W51M, W3 IRS5
linewidth ΔV = 3.5 km/s
G34.3+0.15
JCMT 15-m telescope
H3O+ observations (extragalactic)
364 GHz transition
M82
Arp 220 van der Tak et al. 1992
then Δμ/μ ~ 3 10-7
local starburst
if 364, 307 GHz line position uncertainties ~ 1 km/s
Conclusions
High precision line position measurements
Δμ/μ ~ 3 10-9 (p-H3O+)
~ 0.01 km/s (Galactic molecular clouds)
~ 1 km/s (extragalactic molecular clouds)
provide with ALMA facilities
~ 10-8 (p-NH3 )Galactic
Δμ/μ ~ 3 10-7 (p-H3O+)
~ 10-6 (p-NH3 )extragalactic