Miguel Chávez Dagostino
LMT/GTM Project Scientist - México
Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), Tonantzintla, México
Large Millimeter Telescope -Alfonso Serrano
The puerepechas
Puerto Vallarta
Pico de Orizaba
5740 m; 18832 ft
GTM / Sierra Negra
4600m; 15091 ft
Large Millimeter Telescope (LMT)
• bi-national project: INAOE (Mexico) & UMASS (USA)
• 50-m main reflector (180 panel segments)
• active primary surface r.m.s. of ~75 microns(compensates for gravity & thermal deformations)
• operational wavelengths 0.85 - 4 mm
• beam resolution (FWHM) 4 -18 arcsec
• FOV ~ 4 arcmin diameter
• site: Sierra Negra (4600m, 15100ft); Lat. +19
• LMT shared–risk Early Science > 2014
• Scientific Operation as competitive 32-m LMT
• unique facility when 50-m LMT complete Jan. 2018
LMT primary reflector (M1)
32m
41m
50m
32m
41m
Ring 3
Ring 1
Ring 2
LMT commissioning & 1st-light scientific instrumentation
• AzTEC (P.I. Grant Wilson - UMASS)
• 1.1mm camera (144 pixels - bolometers)
• SiNi spider-web mesh, NTD Ge thermistors
• 100 sq. arcmin/hr/mJy2 (~ SCUBA2 )
• wide-field & confusion-limited continuum mapping
• operational JCMT(2005), ASTE (2007-2008), LMT 32-m (>2014)
• Redshift Seach Receiver (P.I. Neal Erickson - UMASS)
• 2 pixels (dual-pol) – 1 KHz beam-switch
• 75 – 111 GHz instantaneous bandwidth; 31MHz (~100 km/s resolution) at 90GHz;
• Analog auto-correlator
• Receiver temp ~ 60K; stable baselines
• detect multiple molecular-lines without prior information on galaxy redshift
• operational FCRAO-14m (2007-2008), LMT 32-m (>2014)
LMT 32-m – scientific operation
Daniel Rosa et al.
LMT RSR 3mm spectra of bright, lensed Planck-detected SMGsLowenthal et al. (2017)
“A strongly amplified dusty star-forming galaxy at z = 6: unveiling an elusive population of galaxies”
Jorge Zavala et al. 2017, Nature (Astronomy, accepted)
corrected SFR (μ=9.3) ≈ 380 M
/yr, comparable to local ULIRGS
z=6.0269G09.83808
LMT / RSR
Black Hole HuntersAiming to make the first portrait of the hungry monster at the center
of our galaxy, astronomers built “a telescope as big as the world.”
June 8, 2015 http://www.nytimes.com/2015/06/09/science/black-hole-event-horizon-telescope.html
Event Horizon Telescope
ALMA
SMA LMT
1.3mm EHT VLBI 08/04/16 UT
Detecting the black hole shadow
The Event Horizon Telescope
Telescope Diameter (meters) Site Altitude
ALMA 50 x 12m Atacama Desert, Chile 5000m
NOEMA 8 x 15m / 12 x 15m (>2019) Plateau de Bure, France 2550m
SMA 8 x 6m Mauna Kea, HI, USA 4100m
LMT 32m / 50m (>2018) Sierra Negra, Puebla, Mexico 4600m
IRAM 30m Pico Veleta, Granada, Spain 2850m
JCMT 15m Mauna Kea, HI, USA 4092m
APEX 12m Atacama Desert, Chile 5100m
GLT 12m (>2018) Greenland Ice Sheet 3210m
SPT 10m South Pole, Antarctica 2800m
SMT 10m Mount Graham, AZ, USA 3200m
An Anchor Station of the EHT
SPT
ALMA
APEXAPEX
The Event Horizon Telescope
JCMT
15000 km
IRAM 30m NOEMA
12000 km
¿ 10 micro arcsec (μas) ?
384,400 km
20 μas
4 cm
Virgo Cluster – M87 (Virgo A) SMBH ≈ 6 billion solar mass
Schmidt Telescope, Guillermo Haro 1950
Cabeza de Caballo: 1500 años luzConstelación de Orión
VEGA: 1984
TUPURI
Study of Circumstellar (Debris) disks with the GTM/LMT
It all started with Alpha-Lyrae
(Aumann et al. 1984). IRAS
detected an IR excess well
above the expected emission
from the photosphere
IR Excess
Maximum emission at different wavelengths.
Different excess amplitudes. Incidence: 20% in main
sequence stars at MIR, FIR, and (sub-)mm wavelengths
Protoplanetarydisk
Warm transition disk
Modeling the Disk
Emission
Williams & Cieza, 2011
Wyatt, 2008
Cold transition disk Debris disk
~500-200 K ~200-100 K
~100-20 K ~50-20 K
~8 μm ~20 μm
~100 μm~50 μm
TUPURI: EE-The starting point
e Eridani is a relatively
young, nearby, Sun-like star with
tage = 850 Myr , d = 3.22 pc, and
spectral type K2 V. Its age and
distance places it as one of the
closest solar system analogues
where we can study the early
stages in the evolution of a
planetary system similar to our
own. The star is host to a bright,
extended, almost face-on debris
disk, which ranks among the finest
examples of these objects so far
discovered. The star has been
proposed to host two giant
exoplanets at semi-major axes of a
few AU.
Gallery of previous (sub-)mm Observations
SCUBA, SIMBA, SCUBA, SHARCII, MAMBO, SMA, SCUBA2,Greaves et al. (1998), Schutz et al. (2004), Greaves et al. (2005), Backman et al. (2009),
Lestrade & Thilliez (2015), MacGregor et al. (2015)
0.20mJy rms in 18.5hours with tau~0.03@225GHzChavez-Dagostino et al. 2016
Ring inhomogeneities?
VEGA
Arp220 Template created withGRASILSilva et al. (1998) Vega et al. (2008)Ramos et al. (2017)
LMT instrumentation development3mm 2mm 1.4mm 1.1mm 0.85mm
Spectral-line Receivers
RSR 2px, 2 pol
74-111GHz
VLBI (RSR) B4R 1px ALMA 2SBS
125-163GHz
VLBI (EHT)222GHz
Superspec MKIDS
on-chip 190-310 GHz
VLBI
SEQUOIA 16px,
85-115GHz
OMAR 8px 2SBS
210-280 GHz
Continuum Imaging Cameras
AzTEC spiderweb
SiNi +NTD Ge 144px
MUSCAT LEKIDS 1000px
MUSCAT+
TOLTEC+ TOLTEC LEKIDS900px
TOLTEC LEKIDS 1800px
TOLTEC LEKIDS3600px
SCUBA 850um, 0.45mJy r.m.s.confusion limit 2mJy , 5 sources > 3σ
TolTEC 1.1mm, 0.025mJy r.m.s.confusion limit 0.1 mJy , 25000 sources > 3σ
Confusion-limited blank-field surveys
LMT/TolTEC 1.1mm simulation JCMT/SCUBA 850um HDF survey
6 sq. arcmin5” FWHM
50 hours
1800 sq. arcmin
And, what about astrobiology?
• Studies of comets: Deuterium (fractionation)
• Astrochemistry in several stages in the earlyevolution of solar-like stars
• On the T-tau structure of normal stars (vs space UV emission)
• Molecules around mature stars? (49 Ceti)
• Transmission mm-wave spectroscopy?
• Positronium-like experiments (Mauersberger et al.
1996, A&A, 306, 141)?
• Observations of Icy worlds
The Large Millimeter Telescope/El Gran Telescopio Milimétrico:
A New Instrument for Astrobiology
William M. Irvine et al. (2003)
Jonathan Lunine, CornellInternational Astronautical Federation-Guadalajara, Mexico 2016
Searching for biomarkers
EnceladusCassini (INMS+UVS)
Wooten et al. (2015)
Fountains of Enceladus
ALMA Beam
Observing Enceladus with the LMT
Goals:
• Search for molecules whose presence has been evidenced by Cassini
• Search for more (perhaps more complex) species
• Monitor for potential molecular emissionvariability (as a Mission support project)
• Develope ATL for water observations from theground (183GHz)
Observable molecules with LMT
Based on the mass fractions of Waiteet al. 2009), a column density ofwater of Hansen et al. (2011-UVS;NH2O =1 x 1016 cm-2) and assuming LTEand optically thin transitions, we findthat:
H2CO, CO, CH3OH, H2S, HCN, CH3CCH (C3H4), and H2O
are detectable down to an rms~0.15 mK (O. Vega)
Molecule MHz transition TR
----------------------------------------------------------------H2CO
218222.195 *3(0,3)-2(0,2) 4.0 225697.781 *3(1,2)-2(1,1) 5.0
CO115271.202 1-0 60.0 230538.000 2-1 70.0
CH3OH107013.770 *3(1,3)-4(0,4) A++ 4.5 229758.811 *8(-1,8)-7(0,7) E 10.6240938.94 *5(0,5)-4(0,4) A++ t=2 10.3240952.07 *5(2,4)-4(2,3) E t=2 10.5 250924.342 *11(3,8)-11(2,9) A-+ 50.1252252.807 *10(3,8)-10(2,9) A+- 55.9
H2S216710.437 *2(2,0)-2(1,1) 0.32
HCN88631.8473 *1-0 F=2-1 17.2
265886.431 *3-2 20.
C3H4102546.023 *6(1)-5(1) 0.29
102547.983 *6(0)-5(0) 0.33
H2O183310.087 *3(1,3)-2(2,0) 10. 0
And so on…………………………….
@3 and 1mm (SEQUOIA and OMAR,85-115.6GHz, 210-280GHz + ATL)
Enceladus from the groundIRAM [email protected]
Drabek-Maunder et al. (2017, IJA submitted)
50x more methanol than that derived from INMS on Cassini !!
Puerto Vallarta: A Town of Science (??)PV IV- Astrochemistry, Astrobiology and the Origin of Life (March 2019)
• 50x the mass of methanol derived from INMS on Cassini
AlfaCen A-ALMA
A Singularity, a Black Hole
singularity
Event HorizonPhysical manifestation of a mathematical
solution to Einsteins Field Equations
predicting a singularity
VEGA
Actividad magnética en estrellas tipo solarUV vs mm
Vernazza, Avrett, Loeser (1973,1981)
TUPURIDiscos de DEBRIS con el GTM 50-m
Programas desde el espacio:
•Spitzer: FEPS (Carpenter et al. 2005, 2008, 2009)•Herschel: DUNES (Eiroa et al. 2010)
DEBRIS (Matthews & Greaves Co-PIs)•AKARI: (Fujiwara et al. 2009)•WISE (Wright et al. 2010): Kepler transits
Kennedy and Wyatt (2012)
Desde Tierra:Wyatt et al. (2003)Holmes et al. (2003) Liu et al. (2004)Carpenter et al. (2005)Greaves et al. (2005)Nilson et al. (2010)Etc.
SUNS:SCUBA-2 Unbiased Nearby Star Survey; Matthews et al. 2007, Phillips et al. 2009, •500 stars (A, F, G, K, and M), •390h, 356 stars in common with
Herschel DEBRIS program
SONS: SCUBA-2 Observations of Nearby Stars: awarded 270h of Legacy time (2012-2014)
Épsilon Eridani: Muy popular en Ciencia Ficción
•Por su nombre•Por su cercanía•Por sus parámetros (parecidos al Sol)•Por posible presencia planetaria•En literatura, Cine, Televisión, videojuegos, etc.
IMAGING SMBHs WITH THE EVENT HORIZON TELESCOPE & THE LARGE MILLIMETER TELESCOPE
VLBI imaging of a SMBH
LMT Technical Review - Telescope Completion Plan
Motivation for global 1mm VLBI withthe Event Horizon Telescope
• Still need a factor 3 to 5 improvement in
resolution compared to 3.5mm (86 GHz) VLBI
– Wavelength benefit: x 2.5 to x 4
• VLBI observations at λ=1.4mm (current) to 0.85mm (future)
– Extended maximum baselines: x 1.5
• VLBA: 8000km Mauna Kea, HI to St. Croix, US. Virgin Islands
• EHT for Sgr A*: 12000km SPT-LMT, 15000km SPT-NOEMA
– VLBI super-resolution: x 2
Imaging a SMBH
• To resolve BH shadow at 1.3mm
– telescope D (10μas) ~13,000 km
i.e. earth-sized telescope requiredwith beam-size of a few RSch
SMBH BH shadow diameter (μ arcseconds)
a = 0 (no spin) a = 1 (spin)
Sgr A* 53 46
M87* 37 32
Gran Telescopio Milimétrico Alfonso Serrano
Miguel Chávez Dagostino
LMT/GTM Project Scientist - México
Instituto Nacional de Astrofísica, Óptica y Electrónica
Veli Lošinj, Croatia 2017