AUS-CITY Message Forums

The following sections have been updated in the past 3 days.
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-- FIRES (1 updated event, 1 new image) --

FIRE SEASON IN THE WESTERN UNITED STATES
As temperatures became warmer and drier with the arrival of summer, fire season picks up in the Western United States.

* Fires ablaze in northeastern Utah (Image from Sep 19, 2018; Posted Sep 21, 2018)
https://earthobservatory.nasa.gov/images/92800/fires-ablaze-in-northeastern-utah/?src=nha


-- VOLCANOES (1 updated event, 1 new image) --

ACTIVITY AT KRAKATAU
After weeks of moderate activity, satellites captured imagery of an explosive ash plume at the volcanic island of Krakatau.

* Activity at Krakatau (Image from Sep 24, 2018; Posted Sep 24, 2018)
https://earthobservatory.nasa.gov/images/92806/activity-at-krakatau/?src=nha


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Natural Hazards is a service of NASA's Earth Observatory.
http://naturalhazards.nasa.gov/ http://earthobservatory.nasa.gov/

If you have any questions or comments, please contact us:

http://earthobservatory.nasa.gov/contact/

September 21, 2018
MEDIA ADVISORY M18-140
Houston Medical Students to Speak Live with NASA Astronaut on Space Station
NASA astronaut Serena Auñón-Chancellor replaces a high-definition television camera inside Japan's Kibo laboratory module.
NASA astronaut Serena Auñón-Chancellor replaces a high-definition television camera inside Japan's Kibo laboratory module on Sep. 6. Auñón-Chancellor will speak with medical school students in Houston during via downlink from the International Space Station next week.
Credits: NASA

Medical students from The University of Texas Health Sciences Center (UTHealth) in Houston will speak with an astronaut aboard the International Space Station next week. The Earth-to-space call, part of NASA's Year of Education on Station, will air live on NASA Television and the agency's website.

NASA astronaut Serena Auñón-Chancellor will answer questions about life and work aboard the space station from students at her alma mater UTHealth at 12:50 p.m. EDT Thursday, Sept. 27.

The event will take place in MSB 3.001 of the McGovern Medical School at 6431 Fannin St. in Houston. Media interested in covering the event should contact Deborah Mann Lake at deborah.m.lake@ut.tmc.edu or 713-500-3304.

Linking students directly to astronauts aboard the space station provides unique, authentic experiences designed to enhance student learning, performance and interest in science, technology, engineering and mathematics. Astronauts living in space on the orbiting laboratory communicate with NASA's Mission Control Center in Houston 24 hours a day through the Space Network's Tracking and Data Relay Satellites (TDRS).

Follow NASA astronauts on social media at:

https://www.twitter.com/NASA_astronauts

See videos and lesson plans highlighting research on the International Space Station at:

https://www.nasa.gov/stemonstation

-end-


Press Contacts

Katherine Brown
Headquarters, Washington
202-358-1288
katherine.m.brown@nasa.gov

Carla Santiago
Johnson Space Center, Houston
281-483-7150
carla.a.santiago@nasa.gov

GPS OPERATIONAL ADVISORY 267
SUBJ: GPS STATUS 24 SEP 2018

1. SATELLITES, PLANES, AND CLOCKS (CS=CESIUM RB=RUBIDIUM):
A. BLOCK I : NONE
B. BLOCK II: PRNS 1, 2, 3, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15
PLANE : SLOT D2, D1, E1, E3, D4, A4, C3, F3, E2, D5, B4, F6, F5, F2
CLOCK : RB, RB, RB, RB, RB, RB, CS, RB, RB, RB, RB, RB, RB, RB
BLOCK II: PRNS 16, 17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29
PLANE : SLOT B1, C4, D6, C5, E4, D3, E6, F4, A1, B2, B5, C2, B3, C1
CLOCK : RB, RB, RB, RB, RB, RB, RB, RB, CS, RB, RB, RB, RB, RB
BLOCK II: PRNS 30, 31, 32
PLANE : SLOT A3, A2, F1
CLOCK : RB, RB, RB

2. CURRENT ADVISORIES AND FORECASTS :
A. FORECASTS: FOR SEVEN DAYS AFTER EVENT CONCLUDES.
NANU MSG DATE/TIME PRN TYPE SUMMARY (JDAY/ZULU TIME START - STOP)

B. ADVISORIES:
NANU MSG DATE/TIME PRN TYPE SUMMARY (JDAY/ZULU TIME START - STOP)

C. GENERAL:
NANU MSG DATE/TIME PRN TYPE SUMMARY (JDAY/ZULU TIME START - STOP)

2014038 241350Z APR 2014 GENERAL /-/
2014039 271351Z APR 2014 GENERAL /-/
2017122 272144Z NOV 2017 GENERAL /-/
2018010 052217Z MAR 2018 GENERAL /-/

3. REMARKS:
A. THE POINT OF CONTACT FOR GPS MILITARY OPERATIONAL SUPPORT IS THE GPS
OPERATIONS CENTER AT 719-567-2541 OR DSN 560-2541.
B. CIVILIAN: FOR INFORMATION, CONTACT US COAST GUARD NAVCEN AT
COMMERCIAL 703-313-5900 24 HOURS DAILY AND INTERNET
HTTPS://WWW.NAVCEN.USCG.GOV
C. MILITARY SUPPORT WEBPAGES CAN BE FOUND AT THE FOLLOWING
HTTPS://GPS.AFSPC.AF.MIL/GPS OR HTTPS://GPS.AFSPC.AF.MIL/GPSOC

GPS OPERATIONAL ADVISORY 265
SUBJ: GPS STATUS 22 SEP 2018

1. SATELLITES, PLANES, AND CLOCKS (CS=CESIUM RB=RUBIDIUM):
A. BLOCK I : NONE
B. BLOCK II: PRNS 1, 2, 3, 5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15
PLANE : SLOT D2, D1, E1, E3, D4, A4, C3, F3, E2, D5, B4, F6, F5, F2
CLOCK : RB, RB, RB, RB, RB, RB, CS, RB, RB, RB, RB, RB, RB, RB
BLOCK II: PRNS 16, 17, 18, 19, 20, 21, 22, 23, 24, 25, 26, 27, 28, 29
PLANE : SLOT B1, C4, D6, C5, E4, D3, E6, F4, A1, B2, B5, C2, B3, C1
CLOCK : RB, RB, RB, RB, RB, RB, RB, RB, CS, RB, RB, RB, RB, RB
BLOCK II: PRNS 30, 31, 32
PLANE : SLOT A3, A2, F1
CLOCK : RB, RB, RB

2. CURRENT ADVISORIES AND FORECASTS :
A. FORECASTS: FOR SEVEN DAYS AFTER EVENT CONCLUDES.
NANU MSG DATE/TIME PRN TYPE SUMMARY (JDAY/ZULU TIME START - STOP)

B. ADVISORIES:
NANU MSG DATE/TIME PRN TYPE SUMMARY (JDAY/ZULU TIME START - STOP)

C. GENERAL:
NANU MSG DATE/TIME PRN TYPE SUMMARY (JDAY/ZULU TIME START - STOP)

2014038 241350Z APR 2014 GENERAL /-/
2014039 271351Z APR 2014 GENERAL /-/
2017122 272144Z NOV 2017 GENERAL /-/
2018010 052217Z MAR 2018 GENERAL /-/

3. REMARKS:
A. THE POINT OF CONTACT FOR GPS MILITARY OPERATIONAL SUPPORT IS THE GPS
OPERATIONS CENTER AT 719-567-2541 OR DSN 560-2541.
B. CIVILIAN: FOR INFORMATION, CONTACT US COAST GUARD NAVCEN AT
COMMERCIAL 703-313-5900 24 HOURS DAILY AND INTERNET
HTTPS://WWW.NAVCEN.USCG.GOV
C. MILITARY SUPPORT WEBPAGES CAN BE FOUND AT THE FOLLOWING
HTTPS://GPS.AFSPC.AF.MIL/GPS OR HTTPS://GPS.AFSPC.AF.MIL/GPSOC

Official Space Weather Advisory issued by NOAA Space Weather Prediction Center
Boulder, Colorado, USA

SPACE WEATHER ADVISORY OUTLOOK #18-39
2018 September 23 at 9:36 p.m. MDT (2018 September 24 0336 UTC)

**** SPACE WEATHER OUTLOOK ****

Summary For September 17-23

G1 (Minor) geomagnetic storm levels were reached on 21 Sep and 22 Sep due to coronal hole influence

Outlook For September 24-30

No significant space weather is expected for the outlook period.

Data used to provide space weather services are contributed by NOAA,
USAF, NASA, NSF, USGS, the International Space Environment Services
and other observatories, universities, and institutions. More
information is available at SWPC's Web site http://swpc.noaa.gov

Space Weather Message Code: ALTEF3
Serial Number: 2851
Issue Time: 2018 Sep 23 0942 UTC

CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu
Continuation of Serial Number: 2850
Begin Time: 2018 Sep 12 1730 UTC
Yesterday Maximum 2MeV Flux: 4753 pfu

NOAA Space Weather Scale descriptions can be found at
www.swpc.noaa.gov/noaa-scales-explanation

Potential Impacts: Satellite systems may experience significant charging resulting in increased risk to satellite systems.

Space Weather Message Code: ALTEF3
Serial Number: 2850
Issue Time: 2018 Sep 22 1551 UTC

CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu
Continuation of Serial Number: 2849
Begin Time: 2018 Sep 12 1730 UTC
Yesterday Maximum 2MeV Flux: 10633 pfu

NOAA Space Weather Scale descriptions can be found at
www.swpc.noaa.gov/noaa-scales-explanation

Potential Impacts: Satellite systems may experience significant charging resulting in increased risk to satellite systems.

Space Weather Message Code: ALTEF3
Serial Number: 2849
Issue Time: 2018 Sep 21 0900 UTC

CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu
Continuation of Serial Number: 2848
Begin Time: 2018 Sep 12 1730 UTC
Yesterday Maximum 2MeV Flux: 8309 pfu

NOAA Space Weather Scale descriptions can be found at
www.swpc.noaa.gov/noaa-scales-explanation

Potential Impacts: Satellite systems may experience significant charging resulting in increased risk to satellite systems.

Space Weather News for Sept. 20, 2018
http://spaceweather.com
https://www.facebook.com/spaceweatherdotcom

WHO'S AFRAID OF KILLER ELECTRONS? "Killer electrons" from the Van Allen Belts are raining down on Earth's atmosphere. Last Saturday, students from UCLA launched a pair of satellites they built themselves to monitor this space weather threat. The two healthy cubesats are now orbiting Earth and beaming data to the ground, which ham radio operators around the world can easily receive. Visit today's edition of Spaceweather.com to hear the transmissions and learn more.

Remember, SpaceWeather.com is on Facebook!

This week on HST
HST Programs: February 26 - March 4 2018
Program Number Principal Investigator Program Title
14734 Nitya Kallivayalil, The University of Virginia Milky Way Cosmology: Laying the Foundation for Full 6-D Dynamical Mapping of the Nearby Universe
14767 David K. Sing, The Johns Hopkins University The Panchromatic Comparative Exoplanetary Treasury Program
14784 Evgenya L. Shkolnik, Arizona State University HAZMAT: Habitable Zones and M dwarf Activity across Time
14840 Andrea Bellini, Space Telescope Science Institute Schedule Gap Pilot
14889 Jesus Maiz Apellaniz, Centro de Astrobiologia (CSIC/INTA) Inst. Nac. de Tec. Aero. HD 93 129 A: a new collision of two powerful winds and possibly of their sourcesSprObs
15067 Kris Davidson, University of Minnesota - Twin Cities Eta Carinae's Change of State: The End Game
15069 David Bradley Fisher, Swinburne University of Technology The ages and baryonic masses of clumps in turbulent, clumpy disk galaxies
15071 Cynthia Suzanne Froning, University of Texas at Austin The Mega-MUSCLES Treasury Survey: Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems
15073 Boris T. Gaensicke, The University of Warwick Extreme evolved solar systems (EESS)
15075 Jay Christopher Howk, University of Notre Dame The CGM of Massive Galaxies: Where Cold Gas Goes to Die?
15114 Ruben Sanchez-Janssen, Royal Observatory Edinburgh Star cluster formation in extreme environments: an isolated pair of closely interacting dwarf galaxies
15115 John David Silverman, University of Tokyo Emergence of the supermassive black hole - galaxy mass relations at z > 1
15118 Benny Trakhtenbrot, Eidgenossiche Technische Hochschule (ETH) TESTING THE RELEVANCE OF MERGERS AND ENVIROMENT FOR THE FASTEST GROWING BLACK HOLES IN THE MOST INTENSELY STAR FORMING GALAXIES
15128 Alexander Brown, University of Colorado at Boulder Inner Disk Structure and Transport Mechanisms in the Transitional Disk around T Cha
15133 Peter Erwin, Max-Planck-Institut fur extraterrestrische Physik Solving the Mystery of Galaxy Bulges and Bulge Substructure
15145 Adam Riess, The Johns Hopkins University The Hubble Constant to 1%: Physics beyond LambdaCDM
15146 Adam Riess, The Johns Hopkins University A New Threshold of Precision, 30 micro-arcsecond Parallaxes and Beyond
15157 Elena Sabbi, Space Telescope Science Institute The Primordial Binary Fraction in Trumpler 14: Frequency and Multiplicity Parameters
15170 Michael D. Gregg, University of California - Davis Snapshot Survey of the Globular Cluster Populations of Isolated Early Type Galaxies
15181 David J. V. Rosario, Durham Univ. AGN Before and After: Towards a balanced view of the connection between circumnuclear gas and nuclear black hole activity
15189 David John Wilson, The University of Warwick Post Common Envelope Binaries as probes of M dwarf stellar wind and habitable zone radiation environments
15196 David V. Bowen, Princeton University How Do Inflows and Outflows from Galaxies Create Their Inner Circumgalactic Medium?
15207 Alex Harrison Parker, Southwest Research Institute The Moons of Kuiper Belt Dwarf Planets Makemake and 2007 OR10
15211 Letizia Stanghellini, National Optical Astronomy Observatory, AURA Carbon in dusty, compact Galactic planetary nebulae: A study of AGB evolution and recycling in the Milky Way
15212 Michele Trenti, University of Melbourne The brightest galaxies in the first 700 Myr: Building Hubble's legacy of large area IR imaging for JWST and beyond
15213 David E. Trilling, Northern Arizona University A Pure Parallel survey of the colors of small trans-Neptunian objects to constrain the collisional history of the Outer Solar System
15215 Vardha N. Bennert, Cal Poly Corporation, Sponsored Programs Department A Local Baseline of the Black Hole Mass - Host Galaxy Scaling Relations for Active Galaxies
15242 Lucia Marchetti, Open University SNAPshot observations of the largest sample of lensed candidates in the Equatorial and Southern Sky identified with Herschel
15270 Trent J. Dupuy, Gemini Observatory, Northern Operations The Coolest Sample of Brown Dwarf Dynamical Masses
15275 Karoline Gilbert, Space Telescope Science Institute Securing HST's UV Legacy in the Local Volume: Probing Star Formation and the Interstellar Medium in Low Mass Galaxies
15279 Sean Johnson, Princeton University Unveiling Quasar Fueling through a Public Snapshot Survey of Quasar Host Environments
15328 Jessica Agarwal, Max Planck Institute for Solar System Research Orbital period and formation process of the exceptional binary asteroid system 288P
15344 David Jewitt, University of California - Los Angeles Centaurs and Activity Beyond the Water Sublimation Zone
15350 Walter Peter Maksym, Smithsonian Institution Astrophysical Observatory Resolved BPT Mapping of Nearby AGN
15424 William B. Sparks, Space Telescope Science Institute An intensive ultraviolet imaging campaign for Europa's plumes
15425 Katherine de Kleer, California Institute of Technology Eclipse Observations of Europa's Water Plumes
Selected highlights

GO 15071: The Mega-MUSCLES Treasury Survey: Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary System
SOHO image of an extremely strong solar flare M dwarfs - at least, the subset of M dwarfs known as flare stars - are renowned for possessing extremely active chromospheres and coronae. Their discovery as highly variable objects happened largely by chance. Willem Luyten had noticed in 1924 that certain M dwarfs showed spectroscopic variability, with the occasional appearance of emission lines, while in the early 1940s van Maanen commented that two late-type dwarfs, Gl 412B (WX UMa) and Gl 285 (YZ CMi), had brightened by over a magnitude on a handful of parallax plates. The crucial observations came in 1948, when E.F Carpenter noticed that the fainter component of a wide binary system had brightened by more than 3 magnitudes in a matter of minutes. In the succeeding 50 years, these stars have been subjected to extensive observations, particularly at optical and X-ray wavelengths, and the underlying physical processes are relatively well understood. However, most attention has focused on the more active flare stars, and we still have a relatively uncertain grasp on the flare frequency among less active stars. This issue has acquired increased importance with the realisation that somewhere between 10 and 50% of M dwarfs host planetary systems. As the most populous stars in the Galaxy, this also makes M dwarfs the premier planet hosts. The habitable zones in those systems lie much closer to the parent star, and planets are correspondingly vulnerable to detrimental effects from enhanced UV radiation, particularly short-wavelength UV-C. The upcoming Transiting Exoplanet Survey Satellite (TESS), scheduled for launch in April 2018, is expected to reveal numerous additional exoplanet hosts among the SUn's nearest neighbours. This proposal builds on previos HST programs, notably MUSCLES, by using the Cosmic Origins Spectrograph and the Space Telescope Imaging Spectrograph to obtain UV and optical spectra (1150-5700 Angstroms) of nearby M dwarfs, including a range of spectral types as well as a subset of known exoplanet hosts.

GO 15073: Extreme Evolved Solar Systems
Artist's impression of a comet spiralling in to the white dwarf variable, G29-38 During the 1980s, one of the techniques used to search for brown dwarfs was to obtain near-infrared photometry of white dwarf stars, searching for the infrared excess due to these cool companions. In 1988, Ben Zuckerman and Eric Becklin detected just this kind of excess around the DA white dwarfs, G29-38. However, follow-up observations showed that the excess peaked at longer wavelengths than would be expected for a white dwarf; rather, G 29-38 is surrounded by a dusty disk. Given the orbital lifetimes, those dust particles must be regularly replenished, presumably from rocky remnants of a solar system. G 29-38 stood as a lone prototype for almost 2 decades until a handful of other dusty white dwarfs were identified from Spitzer observations. In subsequent years, a significant number of DA white dwarfs have been found to exhibit narrow metallic absorption lines in their spectra. Those lines are generally attributed to "pollution" of the white dwarf atmospheres. Given that the diffusion time for metals within the atmospheres is short (tens to hundreds of years), the only reasonable means of maintaining such lines in ~20% of the DA population is to envisage continuous accretion from a surrounding debris disk. The Cosmic Origins Spectrograph (COS) is an ideal instrument for probing the abundance of trace elements in white dwarfs atmospheres: more than 70 systems have been observed, with detection rates running at around 50%. The present program is using COS to refine the statistics for such systems, focusing primarily on higher-mass whiite dwarfs that are likely to be the remnants of internediate-mass main-sequence stars.

GO 15146: A New Threshold of Precision, 30 micro-arcsecond Parallaxes and Beyond
The Large Magellanic Cloud The cosmic distance scale and dark energy are two key issues in modern astrophysics, and HST has played a vital role in probing both. On the one hand, HST has been involved in cosmic distance measurements since its inception, largely through the H0 Key Project, which used WFPC2 to identify and photometer Cepheids in 31 spiral galaxies at distances from 60 to 400 Mpc. On the other, HST is the prime instrument for investigating cosmic acceleration by searching for and following Type Ia supernovae at moderate and high redshift. These two cosmological parameters are directly related, and recent years have seen renewed interest in improving the accuracy of H0 with the realization that such measurements, when coupled with the improved constraints from the Cosmic Microwave Background, provide important constraints on cosmic acceleration and the nature of Dark Energy. Previous HST programs have focused on identifying and measuring light curves for cepheids in external galaxies (eg GO 10802 , GO 11570 ) or quantifying the effects of variations in intrinsic stellar parameters, such as metallicity (eg GO 10918 , GO 11297 ). The present program is part of a suite of HST programs that newly-developed observing techniques to focus on nearby Cepheids that form the foundation for the whole distance ladder. Recent programs have used drift-scanning with Hubble to derive accurate astrometry, hence trigonometric parallaxes and reliable distances, and accurate photometry, hence flux measurements, for Galactic Cepheids. This is an obviously area where Gaia will have major impact, adding additional high precision data for numerous stars. The Magellanic Clouds and M31 mark the next steps in the distance scale. Gaia is less effective in direct measurements even for the LMC & SMC Cepheids, but the datasets can be tied together given a consistent photometric system. The present program aims to provide that link by using Hubble to obtain accurate photometry for Cepheids in those systems. The DASH technique will be used to step Hubble across multiple fields during each orbit, using gyro control for pointing, imaging with WFC3 in the F555W and F814W filters with UVIS and F160W filter in the near-infrared.

GO 15207: The Moons of Kuiper Belt Dwarf Planets Makemake and 2007 OR10
HST images of the dwarf planet Eris and satellite Dysnomia The Kuiper Belt consists of icy planetoids that orbit the Sun within a broad band stretching from Neptune's orbit (~30 AU) to distance of ~50 AU from the Sun. Over 500 KBOs (or Transneptunian Objects, TNOs) are currently known out of a population of perhaps 70,000 objects with diameters exceeding 100 km. Approximately 2% of the known KBOs are binary; indeed, 11 of the 15 largest systems have detected satellites. This is a surprisingly high fraction, given the difficulties involved in forming such systems and the relative ease with which they can be disrupted. It remains unclear whether these systems formed from single KBOs (through collisions or 3-body interactions) as the Kuiper Belt and the Solar System have evolved, or whether they represent the final tail of an initial (much larger) population of primordial binaries. Interestingly, some observations suggest that the largest KBOs may be higher density, implying larger masses and a greater ability to retain satellites, potentially accounting for the higher satellite fraction. The present program focuses on two of the largest TNOs - makemake is the seond brightest, and OR10 the third largest; both are more than 1000 km in diameter, and both have satellite moons. Wide-Field Camera 3 will be used to monitor the relative positions, enabling derivation of their orbital properties and hence physical characteristics.
Past weeks:

Cycle 14 observations (from March 13 2006 to June 30 2006)
Cycle 15 observations (from July 1 2006)
Cycle 16 observations (from July 1 2007)
Cycle 17 observations (from July 13 2009)
Cycle 18 observations (from August 30 2010)
Cycle 19 observations (from October 3 2011)
Cycle 20 observations (from October 1 2012)
Cycle 21 observations (from October 1 2013)
Cycle 22 observations (from October 1 2014)
Cycle 23 observations (from October 1 2015)
Cycle 24 observations (from October 1 2016)
Cycle 25 observations (from October 1 2017)

The Hubble Space Telescope
Unlocking the Secrets of the Universe

Daily Report #8104

Period Covered:
08:00 PM September 20, 2018 - 07:59 PM September 21, 2018
(DOY 264/0000z - 264/2359z)
Program Principal Investigator Program Title
Science Observations Scheduled
15080 Carl Melis, University of California - San Diego Is SDSSJ195750.83+340404.4 accreting a planetary core?
15163 Hsiao-Wen Chen, University of Chicago COS Ultraviolet Baryon Survey (CUBS)
15187 Vithal Tilvi, Arizona State University Confirmation of the Most Distant Quasar
15212 Michele Trenti, University of Melbourne The brightest galaxies in the first 700 Myr: Building Hubble's legacy of large area IR imaging for JWST and beyond
15242 Lucia Marchetti, Open University SNAPshot observations of the largest sample of lensed candidates in the Equatorial and Southern Sky identified with Herschel
15279 Sean Johnson, Princeton University Unveiling Quasar Fueling through a Public Snapshot Survey of Quasar Host Environments
15307 Michael Gladders, University of Chicago Building the SPT-HST Legacy: Imaging Massive Clusters to z=1.5
15341 Timothy Heckman, The Johns Hopkins University Testing a New Method for Finding Leaky Galaxies: Implications for the Epoch of Reionization
15428 Christina Hedges, Bay Area Environmental Research Institute Sub-Neptune Atmosphere Characterization in a Multi-Planet System
Calibration Observations Scheduled
14940 Mees Fix, Space Telescope Science Institute FUV Detector Dark Monitor
14948 Tyler Desjardins, Space Telescope Science Institute CCD Daily Monitor (Part 3)
14951 Tyler Desjardins, Space Telescope Science Institute CCD Hot Pixel Annealing
14961 Allyssa Riley, Space Telescope Science Institute STIS CCD Dark Monitor Part 3
14963 Allyssa Riley, Space Telescope Science Institute STIS CCD Bias and Read Noise Monitor Part 2
14979 Heather Kurtz, Space Telescope Science Institute UVIS Bowtie Monitor
14982 Catherine Martlin, Space Telescope Science Institute WFC3 UVIS Daily Monitor C
14999 Ben Sunnquist, Space Telescope Science Institute WFC3 CSM monitor with earth flats
Other Observations Scheduled
12046 David Sahnow, Space Telescope Science Institute COS FUV DCE Memory Dump

M5.0 Earthquake - New Guinea, Papua New Guinea
Preliminary Report Magnitude 5.0
Date-Time

24 Sep 2018 03:42:22 UTC
24 Sep 2018 13:42:22 near epicenter
23 Sep 2018 19:42:22 standard time in your timezone

Location 6.300S 145.786E
Depth 128 km
Distances

8.8 km (5.5 mi) W of Kainantu, Papua New Guinea
50.3 km (31.2 mi) ESE of Goroka, Papua New Guinea
119.3 km (74.0 mi) S of Madang, Papua New Guinea
137.4 km (85.2 mi) NW of Bulolo, Papua New Guinea
140.5 km (87.1 mi) WNW of Lae, Papua New Guinea

Location Uncertainty Horizontal: 8.7 km; Vertical 7.7 km
Parameters Nph = 73; Dmin = 374.9 km; Rmss = 1.30 seconds; Gp = 71°
Version =
Event ID us 2000hj7b