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LEW87 - OH/IR stars without OH masers - Nondetection statistics

Interferometry data

Short title: Lewis et al. (1987)
Authors: Lewis, B. M. Eder, J. Terzian, Yervant
Journal: Astronomical Journal (ISSN 0004-6256), vol. 94, Oct. 1987, p. 1025-1034. Research supported by the National Astronomy and Ionosphere Center.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (0 detection) Non-detection table: Show non-detection table (117 non-detection)

Abstract
Potential OH/IR stars are readily recognized from their far-infrared colors. These are confirmed as OH/IR stars by detecting their 1612 MHz masers. Color selection from the sources listed in the IRAS Point Source Catalog therefore provides an efficient means for identifying new objects. However, this approach is not so efficient with weak sources (S₂₅ < 2 Jy). Color-selected sources with S₂₅ _> 2 Jy that are not associated with OH masers have the same color-color range, the same IR flux range, and a similar galactic distribution to the detections. These sources are explicable as normal OH/IR stars in which the OH maser is being suppressed. This would occur when a star with a circumstellar envelope also has a companion star that is able to disrupt the velocity coherence of the normal masing shell. The detection to nondetection ratio then provides a tool for studying the duplicity of these stars over the whole Galaxy.	Comments: Velocity resolution: 0.91 km/s Upper limit for non-detections: 0.025 Jy (3σ)

Abstract

Potential OH/IR stars are readily recognized from their far-infrared colors. These are confirmed as OH/IR stars by detecting their 1612 MHz masers. Color selection from the sources listed in the IRAS Point Source Catalog therefore provides an efficient means for identifying new objects. However, this approach is not so efficient with weak sources (S₂₅ < 2 Jy). Color-selected sources with S₂₅ _> 2 Jy that are not associated with OH masers have the same color-color range, the same IR flux range, and a similar galactic distribution to the detections. These sources are explicable as normal OH/IR stars in which the OH maser is being suppressed. This would occur when a star with a circumstellar envelope also has a companion star that is able to disrupt the velocity coherence of the normal masing shell. The detection to nondetection ratio then provides a tool for studying the duplicity of these stars over the whole Galaxy.

Comments:
Velocity resolution: 0.91 km/s
Upper limit for non-detections: 0.025 Jy (3σ)

Input tables: Table II
Download as: Table (CSV)
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Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

Tip: Use "Box select" or "Lasso select" to display colour-selected sources in Aladin all-sky view

Tip: Click on some source to look at the different surveys. You must select some surveys in previous page at "View images"

Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from LEW87

Tip: Use "Box select" or "Lasso select" to display velocity-selected sources in Aladin all-sky view

Tip: Click on some source to look at the different surveys. You must select some surveys in previous page at "View images"

Longitude-Velocity Map is taken form Dame, Hartmann & Thaddeus (2001)

Distribution of sources from LEW87 in (l,b) histograms

Display associated data

Group name
Different Line detections
IRAS source	IRAS coordinates (RA, Dec)	IRAS source distance (arcsec)	IRAS flux density (F12,F25,F60,F100)
2MASS source	2MASS coordinates (RA, Dec)	2MASS source distance (arcsec)	2MASS magnituted (J,H,K)
GCVS source	GCVS coordinates (RA, Dec)	GCVS source distance (arcsec)	GCVS parameters
WISE source	WISE coordinates (RA, Dec)	WISE source distance (arcsec)	WISE magnitudes (w1, w2, w3, w4)
Akari IRC source	Akari IRC coordinates (RA, Dec)	Akari IRC source distance (arcsec)	Akari IRC fluxes (S09, S18)
Akari FIS source	Akari FIS coordinates (RA, Dec)	Akari FIS source distance (arcsec)	Akari FIS fluxes (S65, S90, S140, S160)
Continuum source	Continuum coordinates (RA, Dec)	Continuum source distance (arcsec)	Continuum parameters
Bolocam GPS	BGPS coordinates (RA, Dec)	BGPS source distance (arcsec)	BGPS parameters
EGO source	EGO coordinates (RA, Dec)	EGO source distance (arcsec)	EGO parameters
Select all	Select all	Select all	Select all

View images

DSS (optical)	SDSS (optical+NIR)	2MASS (JHK)	WISE (4-22 um)	IRAC (3-8 um)	GLIMPSE 360 (3.6-4.5 um)
AKARI color (60-160 um)	PACS color (70-160 um)	SPIRE color (250-500 um)	ATLASGAL (870 um)	ATLASGAL+Planck (870 um)	Bolocam (1.1 mm)
NVSS (1.4 GHz)	Image size: arcsec (default is 120 arcsec)
	Image size: arcsec (default is 120 arcsec)

DSS colored	2MASS colored	WISE colored
SDSS color	IRAC color I1,I2,I4	GLIMPSE 360
PACS color (70-160 um)	SPIRE color (250-500 um)	NVSS (1.4GHz)
ATLASGAL 870 um	ATLASGAL 870 um + Planck	Bolocam 1.1 mm
UKIDSS K	2MASS K

select MAX(oh_data.ra_hms) as ra_hms,MAX(oh_data.dec_dms) as dec_dms,MAX(oh_data.source_name) as source_name,MAX(oh_data.ra) as ra,MAX(oh_data.dec) as dec,MAX(oh_data.l) as l,MAX(oh_data.b) as b,MAX(oh_data.grp) as grp,MAX(oh_data.vlow) as vlow,MAX(oh_data.vup) as vup,MAX(oh_data.vpeak) as vpeak,MAX(oh_data.vpeak_e) as vpeak_e,MAX(oh_data.vpeak2) as vpeak2,MAX(oh_data.vpeak2_e) as vpeak2_e,MAX(oh_data.dv) as dv,MAX(oh_data.other_name) as other_name,MAX(oh_data.peak) as peak,MAX(oh_data.peak_e) as peak_e,MAX(oh_data.peak2) as peak2,MAX(oh_data.peak2_e) as peak2_e,MAX(oh_data.int) as int,MAX(oh_data.int_e) as int_e,MAX(oh_data.rms) as rms,MAX(oh_data.date) as date,MAX(oh_data.date2) as date2,MAX(oh_data.telescope_ref) as telescope_ref,MAX(oh_data.units) as units,MAX(oh_data.beam) as beam,MAX(oh_data.ref) as ref,MAX(oh_data.list_ref) as list_ref,MAX(oh_data.ascii) as ascii,MAX(oh_data.image) as image,MAX(oh_data.id) as id,MAX(oh_data.date_txt) as date_txt,MAX(oh_data.other_name) as other_name,MAX(oh_data.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(oh_data.line) as line,MAX(oh_data.vrange) as vrange,MAX(oh_data.vpeak) as vpeak,MAX(oh_data.peak) as peak,MAX(oh_data.fwhm) as fwhm,MAX(oh_data.int) as int,MAX(oh_data.rms) as rms,MAX(oh_data.units) as units,MAX(oh_data.units_rms) as units_rms,MAX(oh_data.date_txt) as date_txt,MAX(oh_data.telescope_ref) as telescope_ref,MAX(oh_data.beam) as beam,MAX(oh_data.beam_maj) as beam_maj,MAX(oh_data.beam_min) as beam_min,MAX(oh_data.beam_pa) as beam_pa,MAX(oh_data.ref) as ref,MAX(oh_data.list_ref) as list_ref,MAX(oh_data.ascii) as ascii,MAX(oh_data.image) as image,MAX(oh_data.descr) as descr,MAX(oh_data.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(oh_data.dist) as dist,MAX(oh_data.date_txt) as date_txt,MAX(oh_data.freq) as freq,MAX(line_det) as line_det FROM oh_data  LEFT JOIN all_objects_withmet ON oh_data.grp=all_objects_withmet.group_name  WHERE ref ilike 'LEW87' AND detected=true AND hide=false GROUP BY ref

select oh_data.ra_hms,oh_data.dec_dms,oh_data.source_name,oh_data.ra,oh_data.dec,oh_data.l,oh_data.b,oh_data.grp,oh_data.vlow,oh_data.vup,oh_data.vpeak,oh_data.vpeak_e,oh_data.vpeak2,oh_data.vpeak2_e,oh_data.dv,oh_data.other_name,oh_data.peak,oh_data.peak_e,oh_data.peak2,oh_data.peak2_e,oh_data.int,oh_data.int_e,oh_data.rms,oh_data.date,oh_data.date2,oh_data.telescope_ref,oh_data.units,oh_data.beam,oh_data.ref,oh_data.list_ref,oh_data.ascii,oh_data.image,oh_data.id,oh_data.date_txt,oh_data.other_name,oh_data.other_desc,oh_data.thermal,oh_data.line,oh_data.vrange,oh_data.vpeak,oh_data.peak,oh_data.fwhm,oh_data.int,oh_data.rms,oh_data.units,oh_data.units_rms,oh_data.date_txt,oh_data.telescope_ref,oh_data.beam,oh_data.beam_maj,oh_data.beam_min,oh_data.beam_pa,oh_data.ref,oh_data.list_ref,oh_data.ascii,oh_data.image,oh_data.descr,oh_data.id,oh_data.mjy_flag,oh_data.rms_mjy_flag,oh_data.dist,oh_data.date_txt,oh_data.freq,line_det FROM oh_data   LEFT JOIN all_objects_withmet ON oh_data.grp=all_objects_withmet.group_name  WHERE ref ilike 'LEW87' AND detected=true AND hide=false ORDER BY detected DESC,id