constraint on cosmological variation of the proton-to-electron...

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Constraint on cosmological variation of the proton-to-electron mass ratio from two independent telescopes F. van Weerdenburg, 1, 2 M. T. Murphy, 3 A. L. Malec, 3 L. Kaper, 1, 2 and W. Ubachs 1 1 Institute for Lasers, Life and Biophotonics, VU University Amsterdam, de Boelelaan 1081, 1081 HV Amsterdam, The Netherlands 2 Astronomical Institute Anton Pannekoek, Universiteit van Amsterdam, 1098 SJ Amsterdam, The Netherlands 3 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Victoria 3122, Australia Additional material to this paper In the following pages the full spectrum as observed toward the J2123-005 quasar system with UVES-VLT is presented. The observed spectrum is shown in black, the result of the fitted spectrum in green. The upper trace (in dark blue) shows residuals in the fit regions; these parts of the spectrum were included in the fitting routine; the light horizontal lines mark the ±1σ levels. The green ticks marks give the positions of the H 2 and HD velocity components (note that on this scale not all 5 VCs of the final fit are visible). Blue tick marks indicate Lyman-α forest lines. Red tick marks indicate Fe ii lines, while black tick marks indicate C iv lines, including their velocity structures. The regions for λ> 3415 ˚ A were included in the fit for the purpose of constraining the metal absorption (Fe ii and C iv). Line identifications are shown at the bottom for the H 2 and HD lines, as well as for the metal lines. Regions where a dashed horizontal (red) line is shown indicate adjustment of the continuum or the zero level in the fit.

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Page 1: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

Constraint on cosmological variation of the proton-to-electron mass ratio from twoindependent telescopes

F. van Weerdenburg,1, 2 M. T. Murphy,3 A. L. Malec,3 L. Kaper,1, 2 and W. Ubachs1

1Institute for Lasers, Life and Biophotonics, VU University Amsterdam,de Boelelaan 1081, 1081 HV Amsterdam, The Netherlands

2Astronomical Institute Anton Pannekoek, Universiteit van Amsterdam, 1098 SJ Amsterdam, The Netherlands3Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Victoria 3122, Australia

Additional material to this paper

In the following pages the full spectrum as observed toward the J2123-005 quasar system with UVES-VLT is presented.The observed spectrum is shown in black, the result of the fitted spectrum in green. The upper trace (in dark blue)shows residuals in the fit regions; these parts of the spectrum were included in the fitting routine; the light horizontallines mark the ±1σ levels. The green ticks marks give the positions of the H2 and HD velocity components (notethat on this scale not all 5 VCs of the final fit are visible). Blue tick marks indicate Lyman-α forest lines. Red tickmarks indicate Fe ii lines, while black tick marks indicate C iv lines, including their velocity structures. The regionsfor λ > 3415 A were included in the fit for the purpose of constraining the metal absorption (Fe ii and C iv). Lineidentifications are shown at the bottom for the H2 and HD lines, as well as for the metal lines. Regions where adashed horizontal (red) line is shown indicate adjustment of the continuum or the zero level in the fit.

Page 2: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

2

3040 3041 3042 3043 3044 3045 3046 3047 3048 3049 3050 3051

0.0

0.5

1.0

3050 3051 3052 3053 3054 3055 3056 3057 3058 3059 3060 3061

0.0

0.5

1.0

L9P3

3060 3061 3062 3063 3064 3065 3066 3067 3068 3069 3070 3071

0.0

0.5

1.0

Nor

mal

ized

Flux

L8R1 L8P1 L9R5

3070 3071 3072 3073 3074 3075 3076 3077 3078 3079 3080 3081

0.0

0.5

1.0

L8R2 L9P5 L8R3

3080 3081 3082 3083 3084 3085 3086 3087 3088 3089 3090 3091

Wavelength [A]

0.0

0.5

1.0

L8P3W0R1 W0R0 W0R2 L8R4 W0Q1 W0R3

Page 3: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

3

3090 3091 3092 3093 3094 3095 3096 3097 3098 3099 3100 3101

0.0

0.5

1.0

W0R3 W0Q2 HDL8 W0Q3 L7R0 L7R1

3100 3101 3102 3103 3104 3105 3106 3107 3108 3109 3110 3111

0.0

0.5

1.0

L7R1 W0R5 L7P1 W0P3 L7R2 W0Q4 L7P2

3110 3111 3112 3113 3114 3115 3116 3117 3118 3119 3120 3121

0.0

0.5

1.0

Nor

mal

ized

Flux

W0P4 L7R3 W0Q5 L7P3

3120 3121 3122 3123 3124 3125 3126 3127 3128 3129 3130 3131

0.0

0.5

1.0

HDL7 L7P4FeII1055

3130 3131 3132 3133 3134 3135 3136 3137 3138 3139 3140 3141

Wavelength [A]

0.0

0.5

1.0

L7P4 L6R0 L6R2FeII1055

Page 4: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

4

3140 3141 3142 3143 3144 3145 3146 3147 3148 3149 3150 3151

0.0

0.5

1.0

L6R2 L6P2 L7P5 L6R3

3150 3151 3152 3153 3154 3155 3156 3157 3158 3159 3160 3161

0.0

0.5

1.0

L6P3 L6R4FeII1063

3160 3161 3162 3163 3164 3165 3166 3167 3168 3169 3170 3171

0.0

0.5

1.0

Nor

mal

ized

Flux

L6P4

3170 3171 3172 3173 3174 3175 3176 3177 3178 3179 3180 3181

0.0

0.5

1.0

L5P1

3180 3181 3182 3183 3184 3185 3186 3187 3188 3189 3190 3191

Wavelength [A]

0.0

0.5

1.0

L6P5 L5P2 L5R3 HDL5

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5

3190 3191 3192 3193 3194 3195 3196 3197 3198 3199 3200 3201

0.0

0.5

1.0

HDL5 L5P3 L5R4

3200 3201 3202 3203 3204 3205 3206 3207 3208 3209 3210 3211

0.0

0.5

1.0

L5P4 L4R0

3210 3211 3212 3213 3214 3215 3216 3217 3218 3219 3220 3221

0.0

0.5

1.0

Nor

mal

ized

Flux

L4R0 L4R1 L4P1 L4R2 L5P5

3220 3221 3222 3223 3224 3225 3226 3227 3228 3229 3230 3231

0.0

0.5

1.0

L4P2 L4R3 HDL4 FeII1055

3230 3231 3232 3233 3234 3235 3236 3237 3238 3239 3240 3241

Wavelength [A]

0.0

0.5

1.0

L4P3 L4R4

Page 6: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

6

3240 3241 3242 3243 3244 3245 3246 3247 3248 3249 3250 3251

0.0

0.5

1.0

L4R5 FeII1062

3250 3251 3252 3253 3254 3255 3256 3257 3258 3259 3260 3261

0.0

0.5

1.0

L3R0 L3R1 L3P1 L3R2 L4P5FeII1063 FeII1064

3260 3261 3262 3263 3264 3265 3266 3267 3268 3269 3270 3271

0.0

0.5

1.0

Nor

mal

ized

Flux

HDL3 L3R3

3270 3271 3272 3273 3274 3275 3276 3277 3278 3279 3280 3281

0.0

0.5

1.0

L3P3 L3R4

3280 3281 3282 3283 3284 3285 3286 3287 3288 3289 3290 3291

Wavelength [A]

0.0

0.5

1.0

L3P4 L3R5

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7

3290 3291 3292 3293 3294 3295 3296 3297 3298 3299 3300

0.0

0.5

1.0

L2R0

3300 3301 3302 3303 3304 3305 3306 3307 3308 3309 3310

0.0

0.5

1.0

HDL2 L2P1 L2R2 L3P5 L2P2 L2R3FeII1082 FeII1082

3310 3311 3312 3313 3314 3315 3316 3317 3318 3319 3320

0.0

0.5

1.0

Nor

mal

ized

Flux

3320 3321 3322 3323 3324 3325 3326 3327 3328 3329 3330

0.0

0.5

1.0

3330 3331 3332 3333 3334 3335 3336 3337 3338 3339 3340

Wavelength [A]

0.0

0.5

1.0

L2P4 L2R5

Page 8: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

8

3340 3341 3342 3343 3344 3345 3346 3347 3348 3349 3350 3351

0.0

0.5

1.0

L1R0 L1R1L2P5

L1P1 L1R2

3350 3351 3352 3353 3354 3355 3356 3357 3358 3359 3360 3361

0.0

0.5

1.0

L1P2 L1R3 FeII1097

3360 3361 3362 3363 3364 3365 3366 3367 3368 3369 3370 3371

0.0

0.5

1.0

Nor

mal

ized

Flux

L1P3

3370 3371 3372 3373 3374 3375 3376 3377 3378 3379 3380 3381

0.0

0.5

1.0

L1P4 L1R5

3380 3381 3382 3383 3384 3385 3386 3387 3388 3389 3390 3391

Wavelength [A]

0.0

0.5

1.0

L0R0

Page 9: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

9

3390 3391 3392 3393 3394 3395 3396 3397 3398 3399 3400 3401

0.0

0.5

1.0

L0R1 L0P1 L0R2 FeII1145

3400 3401 3402 3403 3404 3405 3406 3407 3408 3409 3410 3411

0.0

0.5

1.0

L0P2 L0R3

3410 3411 3412 3413 3414 3415 3416 3417 3418 3419 3420 3421

0.0

0.5

1.0

Nor

mal

ized

Flux

L0P3 L0R4

3420 3421 3422 3423 3424 3425 3426 3427 3428 3429 3430 3431

0.0

0.5

1.0

3430 3431 3432 3433 3434 3435 3436 3437 3438 3439 3440 3441

Wavelength [A]

0.0

0.5

1.0

Page 10: Constraint on cosmological variation of the proton-to-electron ...wimu/Publications/PRL-J2123-online...Constraint on cosmological variation of the proton-to-electron mass ratio from

10

4905 4906 4907 4908 4909 4910 4911 4912 4913 4914 4915

0.0

0.5

1.0

CIV1548CIV1548

4915 4916 4917 4918 4919 4920 4921 4922 4923 4924 4925

0.0

0.5

1.0

FeII1608FeII1608 CIV1550CIV1550

6950 6951 6952 6953 6954 6955 6956 6957 6958 6959 6960

0.0

0.5

1.0

Nor

mal

ized

Flux

FeII2344

7065 7066 7067 7068 7069 7070 7071 7072 7073 7074 7075

0.0

0.5

1.0

FeII2383

7165 7166 7167 7168 7169 7170 7171 7172 7173 7174 7175

Wavelength [A]

0.0

0.5

1.0

FeII2344FeII2344

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11

7282 7283 7284 7285 7286 7287 7288 7289 7290 7291 7292

0.0

0.5

1.0

FeII2383FeII2383

7710 7711 7712 7713 7714 7715 7716 7717 7718 7719 7720

0.0

0.5

1.0

FeII2600

7906 7907 7908 7909 7910 7911 7912 7913 7914 7915 7916 7917

0.0

0.5

1.0

Nor

mal

ized

Flux

FeII2587FeII2587

7947 7948 7949 7950 7951 7952 7953 7954 7955 7956 7957 7958 7959

Wavelength [A]

0.0

0.5

1.0

FeII2600FeII2600