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OBSID:
29503
Title:
Where is the Dragonfly going? Measuring the Proper Motion of the PSR J2021+3651 
Investigator:
Jin
Observer:
Jin, Ruolan
Phone:
+886 939229771
Email:
ruolanjin@gmail.com
Target Name:
PSR J2021+3651
Sequence Number:
503417
Instrument:
ACIS-S
Grating:
NONE
SI Mode:
TE_006C8
Raster Scan:
N
Annotated DOT:
AUG1224a

Proposal Number:
24500389
Right Ascension:
305.273
Declination:
36.8513
Status:
observed
Start Date:
2024-08-17 23:18:28
Category:
SN, SNR AND ISOLATED NS
Type:
GO
AO Cycle:
24
Dither Flag:
Y
Y Offset:
0
Z Offset:
0
Est. Count Rate:
0.1
Order-1 Count Rate:

Exposure Time:
12
Time Remaining:
12.176
Reqd Start Time:

Reqd Stop Time:

Period:

Epoch:

Start of Period:

End of Period:

PS Margin:

PE Margin:

Max Segments:
0

ACIS Mode:
TE
Standard?:
No
BEP Mode:
VF
Dropped Chip Count:
1
Optional Chips:
I3
On-Chip Summing?:
No
Row Sum:

Column Sum:

Frame Time:

Subarray Mode:
NONE
Starting Row:
0
Row Count:
1023
Subarray Frame Time:


Duty Cycle?:
No
Cycle Count:
0
Primary Exp Time:

Secondary Exp Time:

Event Filter?:
No
Filter Threshold:

Filter Range:

Bias Requested?:
No
Bias Frequency:

Bias After?:
No
Spatial Window?:
No

Abstract:
We propose an ACIS observation of PSR J2021+3651 for measuring its proper motion. Previous studies assumed that the pulsar is moving from the location of its associated TeV source, which is believed to be the pulsar?s birth site. The inferred pulsar moving velocity based on this agrees with the observed bow-shock structures caused by a supersonically moving pulsar. However, the undisturbed torus and the jets of the pulsar wind nebula suggest a mildly moving pulsar, which contradicts with the fast-moving assumption. Only a direct measurement of the pulsar?s velocity can confirm this. By adopting ?Figure of Merit? method, it will become feasible for measuring proper motion of PSR J2021+3651 between the archival data and a new cycle 24 Chandra observation. 1

Remarks:
In order to include as many common reference stars as possible, the new observation would better avoid the roll angle between 40-150 degrees. Our most preferred roll angle is 330 degrees, just the same as the archival data to achieve the best measurements but NOT strictly necessary. Even with a random roll angle, we can still have at least three reference sources for astrometry correction.

psci Run:
99
Processing Date:
Sep 4 09:18
psci Directory:
/nfs/maaxnew/r3/fn/acis128b/acis128.log
OBSID:
29503
SIM Mode:
ACIS-S
OTG Mode:
NONE
Seq Number:
503417
Target Name:
PSR_J2021+3651
AO:
24
Start VCDU:
1310:000
Start Time (UTC):
230:84864.849
Stop Time (UTC):
231:10652.035
Kilosecs:
12.2
% Frames:
100.0
# CCDs:
S4
# Frames:
3880
# Events:
261534
Events/sec:
21
PSCI errors:
0
% drops:
0.1
Bias Errs:
0
FP Temp:
-114.5
Parameter Block:
0x006c9034
Window Block:
-
# Windows:
0
FEP Mode:
Te5x5
BEP Mode:
F
Start Row:
0
# Rows:
1024
Primary Exposure:
31
Secondary Exposure:
0
Duty Cycle:
0
Summing?:
No
Bias?:
No
Trickle?:
Yes
Bias Run:
98


pgf@space.mit.edu Thu Dec 12 21:19:55 EST 2024