time domain astronomy - hou.usra.edu · cara battersby (moderator) is an assistant professor of...
TRANSCRIPT
Time Domain AstronomyCara Battersby (University of Connecticut), ModeratorBrad Cenko (NASA Goddard Space Flight Center)Julie McEnery (NASA Goddard Space Flight Center)Daryl Haggard (McGill University)
Our Panel
Cara Battersby (moderator) is an Assistant Professor of Astrophysics at the University of Connecticut, specializing in extreme star formation, particularly in our Galactic Center
Brad Cenko is a Research Astrophysicist at NASA Goddard Space Flight Center. He is the PI of the Neil Gehrels Swift Observatory, and part of the Zwicky Transient Facility (ZTF) and Large Synoptic Survey Telescope (LSST) teams
Daryl Haggard is an Assistant Professor of Physics at McGill University, specializing in AGN and their host galaxies, Galactic Center and SgrA*, EM counterparts to GW sources, accretion onto compact objects, multi-wavelength and time domain surveys
Julie McEnery is an Astrophysicist at the NASA Goddard Space Flight Center. She is WIRST deputy Project Scientist and was project scientist for the Fermi Gamma-ray Space Telescope until last Monday.
Our Panel
Exoplanet Person! Expert on your exact research area! and also has the same favorite flavor of ice cream as you!
Knower of all Things! AKA a deity Knower of all Things! AKA a theorist
X X
X X
Our Panel
Exoplanet Person! Such an expert on all the things!
Expert on your exact research area! Thinks all your thoughts and also has the same favorite flavor of ice cream!
Knower of all Things! AKA a deity Knower of all Things! AKA a theorist
X X
X XYou!
Schematic of Transients and Variables
Schematic of Transients and Variables
★ Many science areas
Schematic of Transients and Variables
★ Many science areas★ Multiwavelength
Schematic of Transients and Variables
★ Many science areas★ Multiwavelength★ Need dedicated
wide-field surveys...
Schematic of Transients and Variables
★ Many science areas★ Multiwavelength★ Need dedicated
wide-field surveys...★ ...and fast, detailed
follow-up
Schematic of Transients and Variables
★ Many science areas★ Multiwavelength★ Need dedicated
wide-field surveys...★ ...and fast, detailed
follow-up★ Build for what we
know...
Schematic of Transients and Variables
★ Many science areas★ Multiwavelength★ Need dedicated
wide-field surveys...★ ...and fast, detailed
follow-up★ Build for what we
know...★ … and what we
don’t. Huge discovery space.
Far-IR Variability is mostly untapped● Growth of dust in supernova remnants● Detailed time-monitoring of Solar System objects (comets, asteroids...)● Gravitational wave follow-up● The growth of young stars
Far-IR Variability is mostly untapped● Growth of dust in supernova remnants● Detailed time-monitoring of Solar System objects (comets, asteroids...)● Gravitational wave follow-up● The growth of young stars
Herschel Gould Belt
How do Stars Gain their Mass?
(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
Important for understanding origin of the IMF and how planets form and evolve
Herschel Gould Belt
How do Stars Gain their Mass?
(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
Important for understanding origin of the IMF and how planets form and evolve
Star formation… from a snapshot to a movie
Herschel Gould Belt
How do Stars Gain their Mass?
(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
Important for understanding origin of the IMF and how planets form and evolve
Star formation… from a snapshot to a movie
Herschel Gould Belt
How do Stars Gain their Mass?
(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
Important for understanding origin of the IMF and how planets form and evolve
Star formation… from a snapshot to a movie
● Variability is well-established ○ In mid-IR (e.g. YSOVAR Morales-Calderon+ 2011 and Caratti o Garatti 2011, Safron+ 2015, Fischer+ 2019)○ In Far-IR (e.g. SOFIA, Herschel: Billot+ 2012, )○ In sub-mm (JCMT, Herczeg+ 2017, Johnstone+ 2018a)○ Even extragalactically (Spitzer SAGE survey from Meixner+2006 showed variability in 1% of protoclusters in 3
months, Vijh+ 2009)● Time range of days to years
How do Stars Gain their Mass?
ALMA
(Fischer et al. 2019 White Paper… See also high-mass case in Hunter et al. 2019 White Paper
How do Stars Gain their Mass?
● Variability is well-established ○ In mid-IR (e.g. YSOVAR Morales-Calderon+ 2011 and Caratti o Garatti 2011, Safron+ 2015, Fischer+ 2019)○ In Far-IR (e.g. SOFIA, Herschel: Billot+ 2012, )○ In sub-mm (JCMT, Herczeg+ 2017, Johnstone+ 2018a)○ Even extragalactically (Spitzer SAGE survey from Meixner+2006 showed variability in 1% of protoclusters in 3
months, Vijh+ 2009)● Time range of days to years
HOPS 383 in Orion, Sarfon+ 2015
EC 53 (Yoo+ 2017; Johnstone+ 2018b)
(Fischer et al. 2019 White Paper… See also high-mass case in Hunter et al. 2019 White Paper
How do Stars Gain their Mass?
Need dedicated, high-cadence observations of many stars. Light from protostars peaks in far-IR, making it the most direct tracer of variable accretion
(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
How do Stars Gain their Mass?
Origins is designed to map large areas, quickly, and it can deal with the large dynamic range in Galactic targets.
Herzchel Gould Belt(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
How do Stars Gain their Mass?
Origins is designed to map large areas, quickly, and it can deal with the large dynamic range in Galactic targets.
Herzchel Gould Belt
★ Consider time domain discovery science when designing your missions!
(Fischer et al. 2019 White Paper:2019arXiv190307628F ) Info from Will Fischer, Doug Johnstone, Mike Dunham, Joel Green, Jenny Hatchell….See also high-mass case in Hunter et al. 2019 White Paper
The Ground-Based Time-Domain Context:Optical Surveys
● Wide-area optical imaging surveys are near “saturation”○ Bright (< 18 mag) - TESS 30 min cadence over 2500
deg2, ASAS-SN ~ daily cadence over whole sky○ Medium (< 21 mag) - ZTF, ATLAS, Pan-STARRS
imaging Northern Sky every 2-3 days, BlackGem will do similar in the South in few years
○ Faint (< 24 mag) - LSST imaging Southern Sky every 3-4 days
● Major investments from NASA (TESS, ATLAS) and NSF (ZTF, LSST)
The Ground-Based Time-Domain Context: Radio Surveys
● Next frontier will be at radio wavelengths○ Low-frequency arrays in existence or soon coming
online (LOFAR, CHIME, LWA, …)○ Higher frequencies under development (Square
Kilometer Array Phase 1)○ Sensitive to both coherent and incoherent emission
processes● Many (but not all) projects funded outside US
The Ground-Based Time-Domain Context: Scientific Opportunities
● Wide-area survey instruments at complementary wavelengths (“co-observing”)○ High Energies: Current facilities (Fermi, Swift, INTEGRAL) provide complementarity, but unlikely
to be around for entire 10 year duration of LSST○ Infared: WFIRST (somewhat smaller FOV)○ Ultraviolet: Completely lacking (current largest FOV instrument: 18’ x 18’)○ Co-observing extremely powerful for classification (e.g., relativistic ejecta)
● Multi-wavelength Follow-up○ Target-of-Opportunity capabilities on existing missions○ Most (but not all) large missions not well matched to this science (e.g., JWST)○ Swift lesson: fast slewing, UV/X-ray powerful combination○ Spectroscopy is particularly important need
The IceCube experiment in Antarctica has been observing Astrophysical high energy neutrinos since XXX - Where do they come from?
The answer will unambiguously identify acceleration sites of very high energy protons
Where do the highest energy particles in the Universe come from?
The High Energy Sky seen by Fermi-LAT
The Variable Gamma-ray Sky
TXS 0506+056 in months long outburst
Follow up observations across the EM spectrum
IceCube, Fermi-LAT, MAGIC,
AGILE, ASAS-SN, HAWC,
H.E.S.S, INTEGRAL, Kapteyn,
Kanata, Kiso, Liverpool,
Subaru, Swift, VERITAS, VLA,
Science 2018
Some takeaways
Neither the neutrino nor gamma-ray observation were interesting by themselves
Identification of the counterpart with Fermi relied on knowing the past history of the blazar
Timescales were relatively long - didn’t need to rush, but did need long baseline observations
Getting full science interpretation relied on many observations across the EM spectrum with a mix of large and small facilities
Gravitational Waves and Gamma-ray Bursts
Gravitational waves and GRB
Gamma-ray burst was not especially interesting by itself -humdrum phenomena can be groundbreaking when combined with new observation capabilities
Prompt dissemination of Fermi-GBM GRB enabled rapid identification of the gravitational wave signal
Observations of (nearly) simultaneous short duration phenomena only possible for instruments with large FoV
The X-ray Time Domain Context: Our Poster Child GW170817
● Multiwavelength LCs of GW170817
up to ~30 days post-merger
● Confirms NS merger origin for KNe
● Early peak in the UV and blue LCs
● UV for ”blue” KNe, shock break out
● Kilonova evolves rapidly from blue
to red in photom. and
spectroscopy
● UV spectroscopy offer constraints
on r-process elemental
abundances
The X-ray Time Domain Context: Our Poster Child GW170817
● Multiwavelength coverage up to
~600 days post-merger shows non-
thermal synchrotron
● Fit is for an off-axis (∼30deg)
structured relativistic jet in a low
density medium
● Exquisite PL from radio to X-ray
● No break detected thus far
● Ongoing work to place GW170817
into SGRB context and to search
archives for similar sources
Schematic of Transients and Variables
Schematic of Transients and Variables
Time Domain Deserati in the 2020++
Ground-based GW Detectors for 2020s
LIGO-Virgo O3Public Alerts!GCN, ATEL, GW Events (iPhone)
GW’s Across the Mass Scale
Questions for the coming decade 1. What space missions/wavelengths/modes are critical? Do we need a suite of
missions? Which ones? How soon?2. In addition to space missions, how do we support other necessary capabilities
(cyberinfrastructure, archives, theory)?3. How do we better coordinate with large projects from different funding
agencies?4. How do we handle orders of magnitude difference in relevant timescales
(seconds to years)? How much can we do if we miss the “prompt” emission? Will GW localization be enough?
5. How do we coordinate observatories in space and on the ground? (E.g., monitor LIGO-Virgo high confidence regions, vs. all sky monitors, vs. rapid response, … ?) Are TACs ready?
6. What are the implications for observatory schedulers? Should we support VO standards for visibility/scheduling?
7. What archives must we curate?
Takeaway messages
★ Time domain astronomy is a key future discovery space. ★ All future facilities should be considering the needs of time
domain astronomy … both what we know already, and the open discovery space in wavelength and time baseline.
★ Key needs:○ Dedicated, wide-field survey facilities○ High-resolution, multiwavelength facilities for detailed
follow-up studies