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	J/A+A/713/A60	692		High radial velocity stars abundances (Alazzawi+, 2026) ReadMe+ftp 2026A&A...713A..60A Similar Catalogs Post annotation
1.	J/A+A/713/A60/abund		Stellar parameters and abundances for every element/ion measured (16 rows) metaJ/A+A/713/A60/abund

Simple Constraint List Of Constraints

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Column

Constraint

Explain (UCD)

recno

Record number assigned by the VizieR team. Should Not be used for identification. (meta.record)

Star

(char)

Star identifier, as used in the paper (meta.id;meta.main)

Teff

Adopted effective temperature (phys.temperature.effective)

logg

[cm/s2]

Adopted surface gravity (phys.gravity)

vturb

km/s

Microturbulent velocity, xi (phys.veloc)

[Fe/H]

Derived metallicity from FeI lines (phys.abund)

o_O

⁽ⁿ⁾ Number of individual spectral lines used to derive the abundance of [OI] forbidden line (meta.number)

A(O)

⁽ⁿ⁾ Mean abundance log(N(O)/N(H))+12 (phys.abund)

[O/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(O)-A(O)_{sun} (phys.abund)

s_O

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(O) over the number of lines used (Note 1) (phys.atmol.number)

o_NaI

⁽ⁿ⁾ Number of individual spectral lines used to derive the abundance of NaI (meta.number)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

A(NaI)

⁽ⁿ⁾ Mean abundance log(N(NaI)/N(H))+12 (phys.abund)

[NaI/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(NaI)-A(NaI)_{sun} (phys.abund)

s_NaI

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(NaI) over the number of lines used (Note 1) (phys.atmol.number)

o_MgI

Number of individual spectral lines used to derive the abundance of MgI (meta.number)

A(MgI)

Mean abundance log(N(MgI)/N(H))+12 (phys.abund)

[MgI/H]

Abundance relative to the Sun, A(MgI)-A(MgI)_{sun} (phys.abund)

s_MgI

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(MgI) over the number of lines used (Note 1) (phys.atmol.number)

o_AlI

⁽ⁿ⁾ Number of individual spectral lines used to derive the abundance of AlI (meta.number)

A(AlI)

⁽ⁿ⁾ Mean abundance log(N(AlI)/N(H))+12 (phys.abund)

[AlI/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(AlI)-A(AlI)_{sun} (phys.abund)

s_AlI

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(AlI) over the number of lines used (Note 1) (phys.atmol.number)

o_SiI

Number of individual spectral lines used to derive the abundance of SiI (meta.number)

A(SiI)

Mean abundance log(N(SiI)/N(H))+12 (phys.abund)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

[SiI/H]

Abundance relative to the Sun, A(SiI)-A(SiI)_{sun} (phys.abund)

s_SiI

Line-to-line scatter (standard deviation) of A(SiI) over the number of lines used (Note 1) (phys.atmol.number)

o_CaI

Number of individual spectral lines used to derive the abundance of CaI (meta.number)

A(CaI)

Mean abundance log(N(CaI)/N(H))+12 (phys.abund)

[CaI/H]

Abundance relative to the Sun, A(CaI)-A(CaI)_{sun} (phys.abund)

s_CaI

Line-to-line scatter (standard deviation) of A(CaI) over the number of lines used (Note 1) (phys.atmol.number)

o_ScII

Number of individual spectral lines used to derive the abundance of ScII (meta.number)

A(ScII)

Mean abundance log(N(ScII)/N(H))+12 (phys.abund)

[ScII/H]

Abundance relative to the Sun, A(ScII)-A(ScII)_{sun} (phys.abund)

s_ScII

Line-to-line scatter (standard deviation) of A(ScII) over the number of lines used (Note 1) (phys.atmol.number)

o_TiI

Number of individual spectral lines used to derive the abundance of TiI (meta.number)

A(TiI)

Mean abundance log(N(TiI)/N(H))+12 (phys.abund)

[TiI/H]

Abundance relative to the Sun, A(TiI)-A(TiI)_{sun} (phys.abund)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

s_TiI

Line-to-line scatter (standard deviation) of A(TiI) over the number of lines used (Note 1) (phys.atmol.number)

o_TiII

Number of individual spectral lines used to derive the abundance of TiII (meta.number)

A(TiII)

Mean abundance log(N(TiII)/N(H))+12 (phys.abund)

[TiII/H]

Abundance relative to the Sun, A(TiII)-A(TiII)_{sun} (phys.abund)

s_TiII

Line-to-line scatter (standard deviation) of A(TiII) over the number of lines used (Note 1) (phys.atmol.number)

o_VI

Number of individual spectral lines used to derive the abundance of VI (meta.number)

A(VI)

Mean abundance log(N(VI)/N(H))+12 (phys.abund)

[VI/H]

Abundance relative to the Sun, A(VI)-A(VI)_{sun} (phys.abund)

s_VI

Line-to-line scatter (standard deviation) of A(VI) over the number of lines used (Note 1) (phys.atmol.number)

o_CrI

Number of individual spectral lines used to derive the abundance of CrI (meta.number)

A(CrI)

Mean abundance log(N(CrI)/N(H))+12 (phys.abund)

[CrI/H]

Abundance relative to the Sun, A(CrI)-A(CrI)_{sun} (phys.abund)

s_CrI

Line-to-line scatter (standard deviation) of A(CrI) over the number of lines used (Note 1) (phys.atmol.number)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

o_CrII

Number of individual spectral lines used to derive the abundance of CrII (meta.number)

A(CrII)

Mean abundance log(N(CrII)/N(H))+12 (phys.abund)

[CrII/H]

Abundance relative to the Sun, A(CrII)-A(CrII)_{sun} (phys.abund)

s_CrII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(CrII) over the number of lines used (Note 1) (phys.atmol.number)

o_MnI

Number of individual spectral lines used to derive the abundance of MnI (meta.number)

A(MnI)

Mean abundance log(N(MnI)/N(H))+12 (phys.abund)

[MnI/H]

Abundance relative to the Sun, A(MnI)-A(MnI)_{sun} (phys.abund)

s_MnI

Line-to-line scatter (standard deviation) of A(MnI) over the number of lines used (Note 1) (phys.atmol.number)

o_FeII

Number of individual spectral lines used to derive the abundance of FeII (meta.number)

A(FeII)

Mean abundance log(N(FeII)/N(H))+12 (phys.abund)

[FeII/H]

Abundance relative to the Sun, A(FeII)-A(FeII)_{sun} (phys.abund)

s_FeII

Line-to-line scatter (standard deviation) of A(FeII) over the number of lines used (Note 1) (phys.atmol.number)

o_CoI

Number of individual spectral lines used to derive the abundance of CoI (meta.number)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

A(CoI)

Mean abundance log(N(CoI)/N(H))+12 (phys.abund)

[CoI/H]

Abundance relative to the Sun, A(CoI)-A(CoI)_{sun} (phys.abund)

CoI

Line-to-line scatter (standard deviation) of A(CoI) over the number of lines used (Note 1) (phys.atmol.number)

o_NiI

Number of individual spectral lines used to derive the abundance of NiI (meta.number)

A(NiI)

Mean abundance log(N(NiI)/N(H))+12 (phys.abund)

[NiI/H]

Abundance relative to the Sun, A(NiI)-A(NiI)_{sun} (phys.abund)

s_NiI

Line-to-line scatter (standard deviation) of A(NiI) over the number of lines used (Note 1) (phys.atmol.number)

o_CuI

⁽ⁿ⁾ Number of individual spectral lines used to derive the abundance of CuI (meta.number)

A(CuI)

⁽ⁿ⁾ Mean abundance log(N(CuI)/N(H))+12 (phys.abund)

[CuI/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(CuI)-A(CuI)_{sun} (phys.abund)

s_CuI

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(CuI) over the number of lines used (Note 1) (phys.atmol.number)

o_ZnI

Number of individual spectral lines used to derive the abundance of ZnI (meta.number)

A(ZnI)

Mean abundance log(N(ZnI)/N(H))+12 (phys.abund)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

[ZnI/H]

Abundance relative to the Sun, A(ZnI)-A(ZnI)_{sun} (phys.abund)

s_ZnI

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(ZnI) over the number of lines used (Note 1) (phys.atmol.number)

o_YII

Number of individual spectral lines used to derive the abundance of YII (meta.number)

A(YII)

Mean abundance log(N(YII)/N(H))+12 (phys.abund)

[YII/H]

Abundance relative to the Sun, A(YII)-A(YII)_{sun} (phys.abund)

s_YII

Line-to-line scatter (standard deviation) of A(YII) over the number of lines used (Note 1) (phys.atmol.number)

o_ZrII

Number of individual spectral lines used to derive the abundance of ZrII (meta.number)

A(ZrII)

Mean abundance log(N(ZrII)/N(H))+12 (phys.abund)

[ZrII/H]

Abundance relative to the Sun, A(ZrII)-A(ZrII)_{sun} (phys.abund)

s_ZrII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(ZrII) over the number of lines used (Note 1) (phys.atmol.number)

o_MoI

⁽ⁿ⁾ Number of individual spectral lines used to derive the abundance of MoI (meta.number)

A(MoI)

⁽ⁿ⁾ Mean abundance log(N(MoI)/N(H))+12 (phys.abund)

[MoI/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(MoI)-A(MoI)_{sun} (phys.abund)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

s_MoI

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(MoI) over the number of lines used (Note 1) (phys.atmol.number)

o_BaII

Number of individual spectral lines used to derive the abundance of BaII (meta.number)

A(BaII)

Mean abundance log(N(BaII)/N(H))+12 (phys.abund)

[BaII/H]

Abundance relative to the Sun, A(BaII)-A(BaII)_{sun} (phys.abund)

s_BaII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(BaII) over the number of lines used (Note 1) (phys.atmol.number)

o_LaII

Number of individual spectral lines used to derive the abundance of LaII (meta.number)

A(LaII)

Mean abundance log(N(LaII)/N(H))+12 (phys.abund)

[LaII/H]

Abundance relative to the Sun, A(LaII)-A(LaII)_{sun} (phys.abund)

s_LaII

Line-to-line scatter (standard deviation) of A(LaII) over the number of lines used (Note 1) (phys.atmol.number)

o_CeII

Number of individual spectral lines used to derive the abundance of CeII (meta.number)

A(CeII)

Mean abundance log(N(CeII)/N(H))+12 (phys.abund)

[CeII/H]

Abundance relative to the Sun, A(CeII)-A(CeII)_{sun} (phys.abund)

s_CeII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(CeII) over the number of lines used (Note 1) (phys.atmol.number)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

o_PrII

⁽ⁿ⁾ Number of individual spectral lines used to derive the abundance of PrII (meta.number)

A(PrII)

⁽ⁿ⁾ Mean abundance log(N(PrII)/N(H))+12 (phys.abund)

[PrII/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(PrII)-A(PrII)_{sun} (phys.abund)

s_PrII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(PrII) over the number of lines used (Note 1) (phys.atmol.number)

o_NdII

Number of individual spectral lines used to derive the abundance of NdII (meta.number)

A(NdII)

Mean abundance log(N(NdII)/N(H))+12 (phys.abund)

[NdII/H]

Abundance relative to the Sun, A(NdII)-A(NdII)_{sun} (phys.abund)

s_NdII

Line-to-line scatter (standard deviation) of A(NdII) over the number of lines used (Note 1) (phys.atmol.number)

o_SmII

Number of individual spectral lines used to derive the abundance of SmII (meta.number)

A(SmII)

Mean abundance log(N(SmII)/N(H))+12 (phys.abund)

[SmII/H]

Abundance relative to the Sun, A(SmII)-A(SmII)_{sun} (phys.abund)

s_SmII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(SmII) over the number of lines used (Note 1) (phys.atmol.number)

o_EuII

Number of individual spectral lines used to derive the abundance of EuII (meta.number)

A(EuII)

Mean abundance log(N(EuII)/N(H))+12 (phys.abund)

[EuII/H]

⁽ⁿ⁾ Abundance relative to the Sun, A(EuII)-A(EuII)_{sun} (phys.abund)

s_EuII

⁽ⁿ⁾ Line-to-line scatter (standard deviation) of A(EuII) over the number of lines used (Note 1) (phys.atmol.number)

ALL cols

⁽ⁿ⁾ indicates a possible blank or NULL column

⁽ⁱ⁾indexed column

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