Erin W Gunner H Anna D Shane C Carly L Shane S. Mentor: Sean

Slides:

Advertisements

Similar presentations

Team Taylor Observations with the GBT Candidates When a plot or dataset looks like it has a unknown Pulsar, students submit it to one of the astronomers.

Advertisements

Discovery of a Highly Eccentric Binary Millisecond Pulsar in a Gamma-Ray- Detected Globular Cluster Megan DeCesar (UWM) In collaboration with Scott Ransom.

Team Presentation July 22, Jodrell Bank is the original arboretum for Manchester University. Immediately after World War II, first radio telescope.

Radio and Gamma-Ray Beams from Pulsars R. N. Manchester CSIRO Astronomy and Space Science Australia Telescope National Facility, Sydney Summary Pulse profiles.

Pulsating Pulsars: Adventures Outside the Gridding Iron Susan Booth (VAST), Nick Borowicz (Argo Community HS, Summit, IL), Rob Culbertson (Langley HS,

Preliminary results of giant pulse investigations from Crab pulsar with Radioastron. Rudnitskiy A.G., Popov M.V., Soglasnov V.A. 12 th EVN SYMPOSIUM Cagliari,

B RA:16:45 DEC: -03:17 DM: We used a known pulsar to practice on. You have to do a practice pulsar to make sure that the computers and equipment.

What does do? Mini-project for CSE 260 Qian Peng 15 November 2001 Ref.

Pulsar population overview Dunc Lorimer (WVU) November 2, 2006 The observed sample Spin frequencies > 10 Hz - normal pulsars - recycled objects Current/future.

Dakota Johnson, Tildon Johnson, Kyle Barker Rowan County Senior High School Mentor: Mrs. Jennifer Carter Abstract Data Analysis Acknowledgements Radio.

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Digital Signal Processing.

Pulsing Prizes By: Kyle Wenger and Megan Weaver, (Broadway High School, Broadway, VA) How old might they be? Using the ATNF catalog we have approximated.

Abstract Pulsars are highly magnetized, rotating neutron stars that emit a beam of electromagnetic radiation. The radiation can only be observed when the.

Intro Over this week, we observed using three telescopes (the 40ft, the 20m, and the GBT). We also analyzed pointings for candidates which we observed.

Printed by With the help of scientists and staff at NRAO and WVU, high school students in West Virginia and neighboring states are.

PSR J1400 – 1410 Jessica Pal Rowan County Senior High School Introduction Data Analysis Summary Acknowledgements Results A pulsar is a rapidly rotating.

Mean pulse profiles and spectra at the low frequencies Malov O.I., Malofeev V.M. Malov O.I., Malofeev V.M. Pushchino Radio Astronomy Observatory.

Look, up in the sky! By: Lucas Bolyard, Luis Garcia, and Zach Ewen. Prep Fold Plots Looking at Pointings in the sky Up until this point in time, Team Disney.

Methods for the detection of exosolar planets Astronomical Seminar January 2004 Erik Butz.

MeetingDateMaterial 102/04/2015Penn State PSC Overview 202/11/2015Pulsar Properties 302/18/2015Game Show Review 402/25/2015Poster Assignment Introduction/Summer/

Hulse Team Pulsar Research Adam Kelsey, Consuela Hancock, Magaly Rosales, Cameron Deem, What Exactly Is A Pulsar? A pulsar is a rapidly spinning neutron.

Finding Fast Pulsars Today andTomorrow Pulsar Timing Array - A Nanohertz Gravitational Wave Telescope July 21-23, 2005 Jason Hessels McGill University.

Single Pulse Investigations at the Decameter Range O.M. Ulyanov 1, V.V. Zakharenko 1, V.S. Nikolaenko 1, A. Deshpande 2, M.V. Popov 3, V.A. Soglasnov 3,

Vicky Kaspi, McGill University CIFAR AGM Why Do We Need More Radio Pulsars?  Want to build a `Pulsar Timing Array’ (PTA) to detect gravitational.

Pulsar surveys at Arecibo and Green Bank David Champion Gravity Wave Meeting, Marsfield, Dec 2007.

 Tyler Farrell - Westosha Central High School, WI  Heather Frank - Fort Hill High School, MD  Annie B. Agee - Patrick Henry High School, VA  Emily.

Introduction “Tick, tock, tick, tock.” Clocks help keep us on schedule everyday, but how does our own galaxy keep in time? Pulsar’s are natures very own,

Spin Frequency and Harmonics of Pulsar J Abby Chaffins Spring Valley High School Huntington, West Virginia. Equations Frequency f = Spin Frequency.

Team Lyne Conclusive Presentation Pulsar Search Collaboratory Heather Frank, Tyler Farrell, Annie B. Agee, Emily Dick, Trent McDaniel Caitlin Ahrens &

Who discovered the first pulsar? Jocelyn Bell Pulsars spin fast due to what physics concept?

Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Radio Frequency Interference.

JABAK Pulsar Data Analysis Introduction/Purpose When we arrived in Green bank, we did not know what a pulsar was. Now we know their identifying qualities.

Team Bell Anna, Kris, Cassie, Chandler, Ellen, Firas, Tessa, and Josh An investigation into Pulsar Data collected by the Green Bank Telescope.

The Quiet Skies Project and the IYA Astronomers need dark skies to see the stars, but did you know they also need quiet skies? Learn more about radio astronomy,

Team Hulse James J. Joshua M. Daniel P. Adam P. James M. Shane J.

Team Lyne Delaney Jeanine Pigott Elizabeth Leigh Schmitz Mariah Francine Gnegy Zachary Filmore Ramey Dana Marie Dawley Thomas Eugene Hillenbrand Team Mentor:

Pulsar Search Collaboratory Team Bell Cameron Meador Joey Martinez Erin Fankhanel Evan Graber April Liska Kriston Smith Teachers Mr.Weaver Mrs. Larew.

Hulse Catches the Pulse! PSC Summer Institute 2011 By: Jacob Straley, Jacob Houdyschell, Chandler Smith, Nathan Keithline, Allie Sperry, and student mentor.

Turn Down the Noise ! Team Taylor Nathan, Audrey, Alicia, Ben, Skylar, Josh 2.

Pulsar Search Collaboratory Team Disney Modified Julian Date:

Using the GAVRT Radio Telescope: The SETI Project

Using the GAVRT Radio Telescope: The SETI Project

FRB Backend First Light

Long-Term Timing of Globular Cluster Pulsars

Using the GAVRT Radio Telescope: The SETI Project

David P. Anderson Space Sciences Lab UC Berkeley LASER

Searching FRB with Jiamusi-66m Radio Telescope

Using the GAVRT Radio Telescope: The SETI Project

Using the GAVRT Radio Telescope: The SETI Project

2015 NanoGrav meeting Phil Perillat

LOFAR Beam Formed (BF) Data & Pipeline Overview September 9, 2010

Welcome to the Pulsar Search Collaboratory (PSC)

Radio astronomy at Green Bank

Andy Marx Jason Granstedt Jeremy Thorley Robbie Culbertson

Pulsar Data Search Evaluation

Team Taylor: John, Lori, Casey, Tonia, Joey, Elizabeth, and Lazar

An In-depth Analysis of Radio Astronomy

Pulsar Search Collaboratory

Parkes’ Potential Pulsars

Team Bell Pulsar Analysis

The Hunt for Pulsars Rowan County Pulsar Astronomers Abstract

Pulsar 3: Significant peaks, well above the noise

Pulsar Data II Single-Pulse Plots

Pulsar Data I 1.

Team hulse pulsar collaboration

Amateur Pulsar Detection With EME Equipment

Polarization Properties of an Eclipsing Pulsar

Disney Reaches for the Stars Pulsar Search Collaboratory

Pulsar Data II Single-Pulse Plots

Team Parkes PSC 2011.

Presentation transcript:

Erin W Gunner H Anna D Shane C Carly L Shane S. Mentor: Sean Disney Reaches for the Stars Erin W Gunner H Anna D Shane C Carly L Shane S. Mentor: Sean Carly

Introduction Project: to analyze data collected by the Green Bank telescope and search for pulsars Goals: Identify known pulsars, RFI, and new pulsars Investigate variations in periods Sort noise from significant data Carly

Harmonics in Motion Known Pulsar Info: Dec: -13:54 RA: 09:44 DM: 12.5 Period: 0.57026 Shane

shane

Radio Frequency Interference (R.F.I) Documented in Rogue Gallery as a power line Period ~ 1198 ms Shane s

Known Pulsar J1610-1322 Comparisons: RA and Dec changed slightly from known pulsar in catalogue ~ no change in DM Gunner

GBT Candidates Never before seen at 800 MHz. Not in ATNF New pulsar, named J2013-06 in new drift scan data Never before seen at 800 MHz. Strong pulse profile against noise. Anna D

2013-0650 Comparison Little period change Much clearer lines. In 2007 it was observed at a frequency of 350 MHz and now it was observed at a frequency of 800 MHz. Little period change Anna

GBT Candidates Strong vertical lines in the Sub-band Plot. Low probability of noise. Definitely not a known pulsar. Erin

GBT Comparison Investigation looks more like RFI than 2007 data We were very disappointed. No period change Erin

Conclusions Certainties Uncertainties/Questions About 30 plots with extremely close DM values RFI is present in almost half of the plots examined (47%) Saw 3 known pulsars Uncertainties/Questions Could harmonics be different pulsars? Why is there a difference when the pulsar was observed at 350 MHz and 800 MHz? What can we learn about the pulsar? Carly