C H A N D R A   S C I E N C E   C E N T E R
O B S E R V A T I O N   C A T A L O G

OBSID:
24201
 Title:
Flows of hot Baryons in the Milky Way center: How are fountains & chimneys linked to the Galactic-scale outflow?
Investigator:
Ponti
 Observer:
Anastasopoulou, Konstantina
 Phone:
393756720322
 Email:
konstantina.anastasopoulou@inaf.it
Target Name:
GDHIdp59
 Sequence Number:
901765
 Instrument:
ACIS-I
 Grating:
NONE
 SI Mode:
TE_006E6
 Raster Scan:
N
 Annotated DOT:
MAR1422a

Proposal Number:
22910273
 Right Ascension:
268.535
 Declination:
-27.5198
 Status:
archived
 Start Date:
2022-03-17 16:57:10
Category:
GALACTIC DIFFUSE EMISSION AND SURVEYS
 Type:
GO
 AO Cycle:
22
 Dither Flag:
Y
 Y Offset:
0
 Z Offset:
0
Est. Count Rate:
0.06
 Order-1 Count Rate:

 Exposure Time:
4.333
 Time Remaining:
4.243
 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
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:
Covering a 24 square degrees field at the centre of the Milky Way with 7 ks Chandra exposures will allow us to measure the flows of hot baryons from the core of the Milky Way out into the Galactic halo. This will ultimately allow us to determine the distribution of hot plasma that is feeding into the halo, and to understand whether such an outflow is important for feeding and sustaining the Galactic corona and the circum-galactic medium. In addition to our immediate goal of probing the energy flow out of the central Galaxy, this project will produce a legacy dataset that will be used in the future for multiple purposes, including multi-wavelength and time-domain investigations.

Remarks:
No requirement on the roll angle is placed because the pointing will be overlapping. The coordinates specify the approximate center of the field, which is composed of 6 observations.

psci Run:
167
 Processing Date:
Mar 21 2022
 psci Directory:
/nfs/maaxnew/r3/fe/acis119b/acis119.log
OBSID:
24201
 SIM Mode:
ACIS-I
 OTG Mode:
NONE
 Seq Number:
901765
 Target Name:
GDHIdp59
 AO:
22
Start VCDU:
37297:008
 Start Time (UTC):
076:61481.443
 Stop Time (UTC):
076:65734.369
 Kilosecs:
4.3
 % Frames:
100.0
 # CCDs:
I4
# Frames:
1354
 # Events:
112810
 Events/sec:
26
 PSCI errors:
0
 % drops:
0.1
 Bias Errs:
0
 FP Temp:
-115.6
Parameter Block:
0x006e7034
 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:
164

pgf@space.mit.edu Sat Mar 29 10:37:19 EST 2025