Deep Learning of Astronomical Spectroscopy

Slides:

Advertisements

Similar presentations

CDFS SA12 SA15 Morphologies & Star Formation Histories of Massive Galaxies at z > 1.3 P. McCarthy & The GDDS Team Venice 2006.

Advertisements

Neutral Gas Reservoirs from z=0 to z ~ 5 Neutral Gas Reservoirs from z=0 to z ~ 5 Art Wolfe Marc Rafelski: UCSD Marcel Neeleman: UCSD Michele Fumagali:

Introduction to Astrophysics Lecture 4: Light as particles.

Brightnesses, sizes and motions of stars. Recap Canvas assignment due Friday Project: due Friday 11/21 Campus observatory Emission and absorption lines.

Metals at Highish Redshift And Large Scale Structures From DLAs to Underdense Regions Patrick Petitjean Institut d’Astrophysique de Paris B. Aracil R.

PRESS RELEASE  WHO? Astronomers at UCLA and IPAC using the Keck Observatory. –Team members are Ian McLean (PI), Adam Burgasser, Davy Kirkpatrick (IPAC),

The History of Light: How Stars Formed in Galaxies Kai Noeske European Space Agency/ Space Telescope Science Institute Hubble Science Briefing, 1 Mar 2012.

Astronomy and the Electromagnetic Spectrum

1 Hydrogen in the Milky Way Hydrogen is the most abundant element in our galaxy. The 21-cm Line.

Electromagnetic radiation Recap from last time: Light travels at 300,000 km/s. It is a form of electromagnetic radiation. Beyond the range of what the.

Optimal Photometry of Faint Galaxies Kenneth M. Lanzetta Stony Brook University.

Spectroscopy: and finding out the elements of deep space objects.

Measuring the Gas in Galaxies in the Distant Past Philip Lah Too late. Here comes the SKA.

Copyright © 2010 Pearson Education, Inc. Clicker Questions Chapter 10 Measuring the Stars.

Light. What is Light? The third form of energy The only thing astronomers study Electromagnetic radiation The thing that our eyes detect How radio works.

Lecture 14: Searching for planets orbiting other stars III: Using Spectra 1.The Spectra of Stars and Planets 2.The Doppler Effect and its uses 3.Using.

HI at moderate redshifts Philip Lah Science with MIRA workshop Research School of Astronomy & Astrophysics Mount Stromlo Observatory.

Stellar Spectra Ay16 Lecture 2 Feb 5, The Nearest Star SOHO UV Image.

“Damped Lyman Alpha Systems” by Wolfe, Arthur M., Gawiser, E. and Prochaska, Jason X. Jean P. Walker Rutgers University Galaxy Formation Seminar.

The Nature of Light In Astronomy. Herschel’s Infrared experiment Invisible (to our eyes) light immediately beyond the color red is call infrared light.

Teaching Science with Sloan Digital Sky Survey Data GriPhyN/iVDGL Education and Outreach meeting March 1, 2002 Jordan Raddick The Johns Hopkins University.

1 High-z galaxy masses from spectroastrometry Alessio Gnerucci Department of Physics and Astronomy University of Florence 13/12/2009- Obergurgl Collaborators:

Star Properties studied so far… Period Mass Eccentricity Red shift Velocity Temperature (Wiens Law) Composition – which elements and how much of each Color.

Massive galaxies at z > 1.5 By Hans Buist Supervisor Scott Trager Date22nd of june 2007.

Application of Gravitational Lensing Models to the Brightest Strongly Lensed Lyman Break Galaxy – the 8 o’clock arc E. Buckley-Geer 1, S. Allam 1,2, H.

The Foundations of Astronomy Ashley Peter. Redshift The Universe.

+ Criteria for Candidates Altitude > 40°; Apparent Magnitude > 14; Available Distance and Angular Radius; Available Spectra Criteria for Candidates Altitude.

Optical Spectroscopy of Distant Red Galaxies Stijn Wuyts 1, Pieter van Dokkum 2 and Marijn Franx 1 1 Leiden Observatory, P.O. Box 9513, 2300RA Leiden,

Stellar Spectroscopy.

Light and the Electromagnetic Spectrum. Light Phenomenon Isaac Newton ( ) believed light consisted of particles By 1900 most scientists believed.

Radiation Kirchoff’s Laws  Light emitted by a blackbody, a hot opaque body, or hot dense gas produces a continuous spectrum  A hot transparent gas produces.

What can we learn from the luminosity function and color studies? THE SDSS GALAXIES AT REDSHIFT 0.1.

Objectives & Methodology: We aim to identify formerly unknown quasars from select databases, using previously known techniques that have been slightly.

The Foundations of Astronomy Ashley Peter. The Universe

Wide Field Imagers in Space and the Cluster Forbidden Zone Megan Donahue Space Telescope Science Institute Acknowledgements to: Greg Aldering (LBL) and.

1 VVDS: Towards a complete census of star formation at 1.4

Frontiers in Science #7 Co-evolution of Galaxies and Massive Black Holes in the Universe Masayuki Akiyama (Astronomical Institute) 2009/11/25.

Dae-Hee Lee 1, Woong-Seob Jeong 1, Toshio Matsumoto 2,3, Hyung Mok Lee 2, Myungshin Im 2, Bon-Chul Koo 2, Masateru Ishiguro 2, Jonghak Woo 2, Myung Gyoon.

Lecture 1: Introduction to Cosmology Astronomy 5: The Formation and Evolution of the Universe Sandra M. Faber Spring Quarter 2007 UC Santa Cruz.

Student-Faculty Astronomy Research at Swarthmore: Or…doing astronomy research when the Sun is up Professor David Cohen with Victoria Swisher ( ‘ 06), Micah.

Quasars, Galaxies, and Stars…Oh my! Quasars, Galaxies, and Stars…Oh my!! Sarah Turner, Mary Flynn, Andrea Hayden OVERVIEW BACKGROUND Astronomy spectra.

The Prevalence and Properties of Outflowing Galactic Winds at z = 1 Katherine A. Kornei (UCLA) Alice Shapley, Crystal Martin, Alison Coil ETH Zurich February.

Electromagnetic Spectrum. Element Spectrum Each element has a spectral “fingerprint” — a pattern of bright or dark lines that is UNIQUE to that element.

From Avi Loeb reionization. Quest to the Highest Redshift.

Deep Chandra image in the Boötes Field Junxian Wang Johns Hopkins University.

Study Notes for Chapter 30: Stars, Galaxies, and the Universe.

Lecture 3: What the Universe is Made Of Astronomy 5: The Formation and Evolution of the Universe Sandra M. Faber Spring Quarter 2007 UC Santa Cruz.

Reaching for the Stars: My Journey to a Career in Astronomy Pimol Moth Astronomy Instructor Hartnell College.

Cosmological Structure with the Lyman Alpha Forest. Jordi Miralda Escudé ICREA, Institut de Ciències del Cosmos University of Barcelona, Catalonia Edinburgh,

Biased total mass of CC galaxy clusters by SZE measurements Andrea Conte Astronomy PhD, XXIII Cycle “Sapienza” University of Rome. School of Astrophysics.

© 2017 Pearson Education, Inc.

Astronomy Club 2013 Stars – Part 1.

A photometric method to classify high-z supernovae found with HSC

Chandra Science Highlight

NICMOS Measurements of the Near Infrared Background

ASTRONOMICAL DATA ANALYSIS

Spectroscopy Overview

Nobunari Kashikawa （National Astronomical Observatory of Japan）

in a Large-Scale Structure at z=3.1

Possibility of UV observation in Antarctica

Stars and spectral analysis:

How do scientists know what stars and planets are made of?

Astronomy 105 Laboratory Lab 10.

Observational Prospect of NIREBL

The Stellar Population of Metal−Poor Galaxies at z~1

High Resolution Spectroscopy of the IGM: How High

Radiation Kirchoff’s Laws

Quasar quartet embedded in giant nebula reveals rare massive structure in distant universe by Joseph F. Hennawi, J. Xavier Prochaska, Sebastiano Cantalupo,

A modest view of dust at high redshifts

Fig. 1 ALMA spectra showing three detected transitions of C2H3CN.

Presentation transcript:

Deep Learning of Astronomical Spectroscopy J. Xavier Prochaska (UC Santa Cruz) Also starring: D. Parks, S. Dong, Z. Cai, V. Jankov

Who am I? J. Xavier Prochaska Professor of Astronomy & Astrophysics -- Spectroscopist (Former) Astronomer of UC Observatories First-class programmer (I think) Obsessed fan of Deep Learning Poised to dedicate the rest(?!) of my career to this adventure

Spectroscopy Astronomy Astrophysics Discovery, color, shape, location Velocity, composition, density, mass

Spectrum 2D Spectrum (Image) 1D Spectrum (array)

(Large) Spectral Datasets SDSS/BOSS (present) DESI (future) Spectra of ~1 million sources Spectra of ~20 million sources

Hydrogen Atom: “Lyman Alpha” By A_hidrogen_szinkepei.jpg: User:Szdoriderivative work: OrangeDog (talk • contribs) - A_hidrogen_szinkepei.jpg, CC BY 2.5, https://commons.wikimedia.org/w/index.php?curid=6273602

Damped Lya System (Galaxy)

CNN Classification + Spectral Analysis 400 pixel window Parks, X, Dong, Cai 2018

CNN Results Galaxy Surface Galaxy Redshift Density (position) Parks, X, Dong, Cai 2018

New Results CNN learned to ignore sky line Parks, X, Dong, Cai 2018

Peering into the Black Box.. Did the CNN learn the Lorentzian profile?!

SPectral Image Typing (SPIT) Jankov & X 2018

Future Work: U-net for Feature Detection Cai & X 2019

Future Work: GAN for outlier detection X & Huertas-Company 2019

Future Work: RNN for system detection Dong et al. 2019