Cycle 6 Large and Very Large Projects: Abstracts and Targets

We propose a series of observations of the periodic comet 9P/Tempel 1 in conjunction with NASA's Deep Impact mission. This mission is a spacecraft that will release a 370 kg impactor into the nucleus of the comet on July 4, 2005 at high relative velocity. Our primary objective is to study the generation of prompt x-rays in the impact plume and the change in charge exchange created x-rays as the impact ejecta propgates through the neutral coma. To this end we plan to obtain ACIS-S imaging spectroscopy before, during, and following the impact.

LP/VLP	Prop #	Subject Category	PI Name	Title
LP	06100312	SOLAR SYSTEM	Carey Lisse	Comet 9P/Tempel 1 During the Deep Impact Encounter
VLP	06200204	STARS AND WD	Wayne Waldron	A Chandra HETGS Survey of O-Stars
LP	06200294	STARS AND WD	Joel Kastner	The X-ray Spectrum of a Planetary Nebula at High Resolution
LP	06500333	SN, SNR AND ISOLATED NS	Patrick Slane	The Structure and Composition of Pulsar Winds and their Nebulae
VLP	06500496	SN, SNR AND ISOLATED NS	Robert Rutledge	Search for Sub-Millisecond Pulsars in 47 Tuc
LP	06500950	SN, SNR AND ISOLATED NS	Marten van Kerkwijk	Spectra of Neutron Stars with Strongly Magnetized Hydrogen Atmospheres
LP	06800101	CLUSTERS OF GALAXIES	Alexey Vikhlinin	DARK ENERGY WITH X-RAY CLUSTERS: CHANDRA OBSERVATIONS OF 41 HIGH-REDSHIFT CLUSTERS FROM THE 400 d eg^2 ROSAT PSPC SURVEY
LP	06800102	CLUSTERS OF GALAXIES	Alexey Vikhlinin	A CHANDRA TREASURY OBSERVATION OF THE BEST EXAMPLE OF A CLUSTER COLD FRONT
LP	06800613	CLUSTERS OF GALAXIES	William Forman	The History of AGN Activity in M87 and the Interaction of Nuclear Outbursts with the Surrounding Atmosphere
TOO/LP	06900144	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	Fabrizio Nicastro	Continuing X-Raying the Intergalactic Medium with Blazars in Outburst: Deeper in Redshift and Wider in Area.
VLP	06900444	EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS	Kirpal Nandra	Deep Chandra Imaging of the Extended Groth Strip: The Co-evolution of Black Holes and Galaxies
LP	06910168	GALACTIC DIFFUSE EMISSION AND SURVEYS	Leisa Townsley	Massive Star Life, Death, and Rebirth in the Perseus Arm

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
NULL	NULL	9P/Tempel 1	ACIS-S	TE	NONE	25	1.0
NULL	NULL	9P/Tempel 1	ACIS-S	TE	NONE	25	1.0
NULL	NULL	9P/Tempel 1	ACIS-S	TE	NONE	25	1.0
NULL	NULL	9P/Tempel 1	ACIS-S	TE	NONE	25	1.0
NULL	NULL	9P/Tempel 1	ACIS-S	TE	NONE	50	1.0
NULL	NULL	9P/Tempel 1	ACIS-S	TE	NONE	150	1.0

We are requesting HETGS observations of 6 normal O-stars to further explore the characteristics and the origin of the remarkably detailed X-ray line spectra that has been revealed by Chandra. These new targets have been carefully selected on the basis of their normal optical and UV spectra, instead of their X-ray brightness or peculiarity. Along with archival HETGS spectra, this collection will provide complete coverage of the O-star domain in the H-R diagram. The spectra from this unbiased sample will be assembled in a comprehensive X-ray atlas, which will be used to search for morphological trends in the emission lines as a function of stellar parameters. These trends will guide the development of quantitative models to explain the behavior of the X-ray emission lines of O-type stars.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
06 40 58.70	+09 53 44.70	15 Mon	ACIS-S	TE	HETG	108	0.046400
10 43 57.50	-59 32 51.00	HD93129AB	ACIS-S	TE	HETG	145	0.034100
10 44 45.00	-59 33 54.70	HD93250	ACIS-S	TE	HETG	24	0.025500
10 44 45.00	-59 33 54.70	HD93250	ACIS-S	TE	HETG	170	0.025500
18 03 52.40	-24 21 38.60	9 Sgr	ACIS-S	TE	HETG	147	0.024900

Planetary nebulae (PNs) provide unique insights into a wide range of astrophysical phenomena. X-ray imaging of PNs by CXO has now broken open the study of very high temperature gas in these objects. To make further progress, we require detailed information concerning gas temperature and composition as a function of position within X-ray emitting PN "hot bubbles." Such information can be obtained only from observations combining high spectral and spatial resolution. We propose a 300 ks LETG/ACIS-S exposure of BD+303639, a particularly X-ray-bright PN. Such a deep, high spectral resolution observation of a PN has yet to be attempted. The proposed observation thus represents a potential breakthrough in our understanding of the origin and evolution of PNs.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
19 34 45.20	+30 30 58.90	BD +303639	ACIS-S	TE	LETG	130	0.033000
19 34 45.20	+30 30 58.90	BD +303639	ACIS-S	TE	LETG	170	0.033000

Chandra studies of pulsar wind nebulae have revealed stunning new information on the composition of the winds, the presence of jets and equatorial outflows, and the structure in and around the wind termination shock. Monitoring observations reveal temporal variations in resolved structures that challenge our understanding of particle acceleration and energy flow in these systems. Here we propose deep observations of G54.1+0.3 and PSR B1509-58 in order to probe the complex structure in their interior regions at arcsecond resolution. These observations will allow us to measure the spectrum and morphology of these features in order to constrain models for particle acceleration, the formation and structure of jets, and the geometry of particle flows in PWNe.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
15 13 55.60	-59 08 08.90	PSR B1509-58	ACIS-I	TE	NONE	47.5	8
15 13 55.60	-59 08 08.90	PSR B1509-58	ACIS-I	TE	NONE	47.5	8
15 13 55.60	-59 08 08.90	PSR B1509-58	ACIS-I	TE	NONE	47.5	8
15 13 55.60	-59 08 08.90	PSR B1509-58	ACIS-I	TE	NONE	47.5	8

We propose an observation with the ability to detect multiple isolated sub-millisecond pulsars among the unidentified X-ray sources in 47 Tuc, with significant secondary science. Observations in the X-ray band overcome the limited time resolution of even the best radio observations, allowing for the first time the setting of a new ``speed record'' for pulsars at sub-ms periods, below the now 20-year-old record of P = 1.558 ms. The detection of sub-ms pulsars would rule out equations of state for dense matter, provide even better clocks for their many physics applications, and create a strong impetus for future improvement of observational techniques. The absence of sub-ms pulsars would provide compelling evidence for a spin period limit.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time	Count Rate
00 24 05.20	-72 04 49.90	47 Tuc	HRC-S	NONE	170	0.2
00 24 05.20	-72 04 49.90	47 Tuc	HRC-S	NONE	170	0.2
00 24 05.20	-72 04 49.90	47 Tuc	HRC-S	NONE	170	0.2
00 24 05.20	-72 04 49.90	47 Tuc	HRC-S	NONE	170	0.2
00 24 05.20	-72 04 49.90	47 Tuc	HRC-S	NONE	120	0.2

Proposal Title: Spectra of Neutron Stars with Strongly Magnetized Hydrogen Atmospheres

Neutron stars are unique laboratories for matter at extreme densities and magnetic field strengths. Much of the physics is encapsulated in neutron star spectra, but until recently no suitable sources were known. However, over the last year photospheric absorption features - likely due to hydrogen in strongly magnetized atmospheres - have been found for three nearby neutron stars. We propose to obtain high-quality, 300 ks LETG spectra of the two brightest sources. These data will allow examination of the absorption features and permit searches for other associated features. With detailed understandings of these lines one could measure the surface magnetic fields, compositions and temperatures, eventually leading to direct constraints on the equation of state at supra-nuclear densities.

R.A.	Dec.	Target Name	Det.	Grating	Exp.Time	Count Rate
07 20 25.00	-31 25 50.20	RX J0720.4-3125	HRC-S	LETG	75	1.9
07 20 25.00	-31 25 50.20	RX J0720.4-3125	HRC-S	LETG	75	1.9
07 20 25.00	-31 25 50.20	RX J0720.4-3125	HRC-S	LETG	75	1.9
07 20 25.00	-31 25 50.20	RX J0720.4-3125	HRC-S	LETG	75	1.9

Proposal Title: DARK ENERGY WITH X-RAY CLUSTERS: CHANDRA OBSERVATIONS OF 41 HIGH-REDSHIFT CLUSTERS FROM THE 400 d eg^2 ROSAT PSPC SURVEY

We propose Chandra observations to measure temperature and gas mass in a sample of 41 high-z galaxy clusters from our 400 deg^2 ROSAT survey. This sample is comparable in number to all clusters in the local Universe (z<0.1) above a similar limiting mass, and covers a factor of 3 larger volume at z=0.4-1. Chandra observations will provide the total mass function estimates at =0.4, 0.5, and 0.65, which can be directly compared with the local measurements at =0.05. These data will provide a measurement of the dark energy equation of state via the cluster evolution test which is completely independent from SN Ia and CMB and has different degeneracies. Some targets in this proposal are in common with the HRC GTO proposal 06900018. These programs are not in conflict.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
00 30 33.60	+26 18 16.00	cl0030+2618	ACIS-I	TE	NONE	20	0.03
02 16 33.70	-17 47 27.00	cl0216-1747	ACIS-I	TE	NONE	65	0.03
02 30 26.60	+18 36 22.00	cl0230+1836	ACIS-I	TE	NONE	70	0.03
03 28 36.10	-21 40 04.00	cl0328-2140	ACIS-I	TE	NONE	60	0.03
03 33 10.30	-24 56 40.00	cl0333-2456	ACIS-I	TE	NONE	40	0.03
03 55 59.30	-37 41 46.00	cl0355-3741	ACIS-I	TE	NONE	30	0.03
04 05 24.30	-41 00 15.00	cl0405-4100	ACIS-I	TE	NONE	80	0.03
05 21 10.50	-25 30 36.00	cl0521-2530	ACIS-I	TE	NONE	15	0.03
08 53 13.40	+57 59 44.00	cl0853+5759	ACIS-I	TE	NONE	25	0.03
09 56 02.80	+41 07 08.00	cl0956+4107	ACIS-I	TE	NONE	40	0.03
12 02 13.70	+57 51 53.00	cl1202+5751	ACIS-I	TE	NONE	60	0.03
12 12 19.20	+27 33 13.00	cl1212+2733	ACIS-I	TE	NONE	15	0.03
12 22 01.90	+27 09 19.00	cl1222+2709	ACIS-I	TE	NONE	50	0.03
13 57 19.40	+62 32 42.00	cl1357+6232	ACIS-I	TE	NONE	45	0.03

Proposal Title: A CHANDRA TREASURY OBSERVATION OF THE BEST EXAMPLE OF A CLUSTER COLD FRONT

We propose a 450 ksec observation of A3667, the best example of a cluster cold front. A deep image of the best cold front by the highest angular resolution X-ray telescope will push the study of the physics of the intracluster medium to the limit. Our main goals are 1) to observe the turbulence in the intracluster medium by direct imaging of any perturbations of the front surface; 2) to study transport processes in the ICM using the gas density and temperature profiles across the front with a spatial resolution of 1/5 of the Coulomb mean free path; 3) to characterize the magnetic field structure by mapping the onset of the Kelvin-Helmholtz instability. The proposed deep Chandra image of A3667 will be one of the treasury images of the X-ray astronomy.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
20 12 50.80	-56 50 53.90	Abell 3667	ACIS-I	TE	NONE	110	6.6
20 12 50.80	-56 50 53.90	Abell 3667	ACIS-I	TE	NONE	170	6.6
20 12 50.80	-56 50 53.90	Abell 3667	ACIS-I	TE	NONE	170	6.6

Proposal Title: The History of AGN Activity in M87 and the Interaction of Nuclear Outbursts with the Surrounding Atmosphere

We propose a 500 ksec ACIS-I observation to study the interaction between energy outbursts from the supermassive black hole (SMBH) in M87 and its surrounding gaseous atmosphere. We will inventory the plasma bubbles inflated by the SMBH, search for weak shocks, study the interaction of relativistic plasma in bubbles with the surrounding hot gas, measure turbulence in the cluster gas, study the microphysics of the interaction between the plasma in the bubbles and the surrounding gas, and estimate the gas viscosity by measuring the width of shock fronts. By determining the energy associated with bubbles and shocks, we can chronicle the mechanical power output of the SMBH. Finally we will study particle acceleration and cooling models by measuring inter-knot spectra along the jet.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
12 30 49.50	+12 23 28.00	M87	ACIS-I	CC	NONE	12	27
12 30 49.50	+12 23 28.00	M87	ACIS-I	TE	NONE	160	27
12 30 49.50	+12 23 28.00	M87	ACIS-I	TE	NONE	170	27
12 30 49.50	+12 23 28.00	M87	ACIS-I	TE	NONE	170	27

Proposal Title: Continuing X-Raying the Intergalactic Medium with Blazars in Outburst: Deeper in Redshift and Wider in Area.

We propose to extend our highly succesful Chandra-AO4 and -AO5 TOO programs to the 6th Chandra cycle, to observe up to 2 blazars in exceptionally high states with the Chandra HRCS-LETG (hereinafter HLETG) for a total exposure time of {\bf 340 ks} (2 orbits). We shall dramatically reduce the uncertainty on the cosmological baryon mass density $\Omega_b$ in the local Universe studying the ``warm'', low-redshift, phase of the intergalactic medium (WHIM), where most of the baryonic matter of the $z \ls 1$ Universe is believed to hide.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
NULL	NULL	high-z blazar in outburst	HRC-S		LETG	170	2.5
NULL	NULL	moderate-z blazar in outburst	HRC-S		LETG	170	5.0

Proposal Title: Deep Chandra Imaging of the Extended Groth Strip: The Co-evolution of Black Holes and Galaxies

The Extended Groth Strip (EGS) is a half square degree region that has been targeted intensively for galaxy evolution studies. A remarkable array of ultra-deep data have been or will be accumulated, to include radio, near/mid/far IR, optical and UV data of depth comparable to or better than any part of the sky. It is also the subject of the massive DEEP2 redshift survey, giving high quality Keck spectra for 16-17,000 galaxies. The clear gap in the coverage of the EGS is in the X-ray, and we therefore propose to augment the single deep Chandra pointing with 7 more, to image the whole strip. Our goal is to study the co-evolution of galaxies and black holes, by examining in detail the astrophysics of AGN activity, and its relationship to the host galaxy and surrounding large scale structure.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
14 15 47.50	+52 08 21.40	EGS-7	ACIS-I	TE	NONE	30	0.6
14 15 47.50	+52 08 21.40	EGS-7	ACIS-I	TE	NONE	170	0.6
14 16 49.50	+52 19 57.60	EGS-6	ACIS-I	TE	NONE	30	0.6
14 16 49.50	+52 19 57.60	EGS-6	ACIS-I	TE	NONE	170	0.6
14 18 32.90	+52 38 56.90	EGS-5	ACIS-I	TE	NONE	30	0.6
14 18 32.90	+52 38 56.90	EGS-5	ACIS-I	TE	NONE	170	0.6
14 19 36.40	+52 50 27.70	EGS-4	ACIS-I	TE	NONE	30	0.6
14 19 36.40	+52 50 27.70	EGS-4	ACIS-I	TE	NONE	170	0.6
14 20 40.50	+53 01 56.30	EGS-3	ACIS-I	TE	NONE	30	0.6
14 20 40.50	+53 01 56.30	EGS-3	ACIS-I	TE	NONE	170	0.6
14 21 45.20	+53 13 22.70	EGS-2	ACIS-I	TE	NONE	30	0.6
14 21 45.20	+53 13 22.70	EGS-2	ACIS-I	TE	NONE	170	0.6
14 22 54.80	+53 25 32.50	EGS-1	ACIS-I	TE	NONE	30	0.6
14 22 54.80	+53 25 32.50	EGS-1	ACIS-I	TE	NONE	170	0.6

Proposal Title: Massive Star Life, Death, and Rebirth in the Perseus Arm PI: Leisa Townsley

This joint Chandra/XMM mosaic of W4/W3/HB3 allows us to chronicle the X-ray output of the entire life cycle of high-mass stars, from their intrinsic and wind-collision emission, through their SN phase, and back to the embedded, protostellar X-rays heralding the next generation of massive star formation. In addition we see the feedback of these massive stars on the interstellar medium in the Perseus Arm: the stellar winds from a massive young cluster (IC 1805) have blown the W4 superbubble and chimney; perhaps an older superbubble is over 100 times brighter in X-rays due to supernovae in its interior (HB3), and the expansion of these bubbles is compressing the W3 molecular cloud and triggering a new generation of stars to form.

R.A.	Dec.	Target Name	Det.	Mode	Grating	Exp.Time	Count Rate
02 25 40.60	+62 05 52.40	W3 Main IRS5	ACIS-I	TE	NONE	40	1.0
02 26 50.80	+62 15 52.00	W3 North	ACIS-I	TE	NONE	80	1.0
02 27 04.10	+61 52 22.00	W3(OH)	ACIS-I	TE	NONE	80	1.0

The Chandra X-Ray Center (CXC) is operated for NASA by the Smithsonian Astrophysical Observatory. 60 Garden Street, Cambridge, MA 02138 USA. Email: cxchelp@head.cfa.harvard.edu Smithsonian Institution, Copyright © 1998-2024. All rights reserved.