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 32m@239.74GHz

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